Putting the ''I'' in IHY: The United Nations Report for the International Heliophysical Year 2007 (Studies in Space Policy, 3)

Studies in Space Policy Volume 3

Edited by the European Space Policy Institute Director: Kai-Uwe Schrogl

Editorial Advisory Board: Herbert Allgeier Alvaro Azcarraga Frances Brown Alain Gaubert Leen Hordijk Peter Jankowitsch Ulrike Landfester Andre Lebeau Jan-Baldem Mennicken Alfredo Roma

Barbara J. Thompson, Natchimuthuk Gopalswamy, Joseph M. Davila, Hans J. Haubold (eds.)

Putting the "I" in IHY The United Nations Report for the International Heliophysical Year 2007

SpringerWienNewYork

Barbara J. Thompson Heliophysics Science Division NASA/GSFC Greenbelt, MD, USA

Natchimuthuk Gopalswamy Heliophysics Science Division NASA/GSFC Greenbelt, MD, USA

Joseph M. Davila Heliophysics Science Division NASA/GSFC Greenbelt, MD, USA

Hans J. Haubold UN Office for Outer Space Affairs Vienna, Austria This work is subject to copyright. All rights are reserved, whether the whole or part of the material is concerned, specifically those of translation, reprinting, re-use of illustrations, broadcasting, reproduction by photocopying machines or similar means, and storage in data banks. Product Liability: The publisher can give no guarantee for all the information contained in this book. This does also refer to information about drug dosage and application thereof. In every individual case the respective user must check its accuracy by consulting other pharmaceutical literature. The use of registered names, trademarks, etc. in this publication does not imply, even in the absence of a specific statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use.  2009 Springer-Verlag/Wien Printed in Germany SpringerWienNewYork is a part of Springer Science þ Business Media springer.at Typesetting: Thomson Press (India) Ltd., Chennai Printing: Strauss GmbH, 69509 M€orlenbach, Germany Cover: “Composite design courtesy of European Science Foundation”. Printed on acid-free and chlorine-free bleached paper SPIN: 12641345

With 164 Colour and 14 Black & White Figures Library of Congress Control Number: 2009931219

ISSN 1868-5307 ISBN 978-3-211-99179-4 SpringerWienNewYork

Preface Putting the “I” in IHY This book is about international cooperation. It demonstrates how the power of scientific imagination and investigation can bring together people form all continents in almost all countries around the globe. In presenting this impressive result, we can understand, how much unifying force the quest for understanding our universe and using outer space for that purpose have. Astronomy is far away from being a “political” area of science. But is has enormous political effects – and all of these effects are positive. This book about the international aspects and achievements of the “International Heliophysical Year (IHY) 2007” can be regarded as a compendium of the fertile impacts of conducting research in this field. The main focus, as the title implicates, is the international cooperation, which has emerged from this grassroots initiative. North and South, industrialized and developing countries have been coordinating their efforts and have been learning from each other in a mutual partnership under a joint understanding of sharing the scientific benefits. Through this, trans-border networks have been created and scientific as well as cultural exchange took place. Another focus of the book shows, how much astronomy contributes to the basis of knowledge society as today’s concept for mastering the future. Astronomy has been and will be attracting large numbers of young people to enter an education and career in science and engineering. Such attractions we desperately need in all countries around the world, and we have to be glad about initiatives like IHY, which are successful in raising awareness, interest and fascination. This book is therefore particularly well placed in the series “Studies in Space Policy”, since it highlights the policy needs for space education as well as international cooperation in a most dedicated and convincing way. Kai-Uwe Schrogl Director European Space Policy Institute (ESPI)

v

Biographical sketch: Professor Dr. Hans J. Haubold Education Diploma, Physics, Technical University Chemnitz, 1974, Germany Ph.D., Astrophysics, Institute for Astrophysics, 1980, Potsdam, Germany D.Sc., Astrophysics, Institute for Astrophysics, Potsdam, 1984, Germany Research Professor, Theoretical Astrophysics, Berlin, 1988, German Academy of Sciences

IHY Roles Implementation of the United Nations Basic Space Science Observatory Development Programme for IHY 2007 Dr. Hans J. Haubold is pursuing research in astrophysics and co-authored four books, on nuclear astrophysics (with A. M. Mathai, Akademie-Verlag, Berlin, 1988), on the early universe and formation of structure (with S. Gottloeber, J. P. Muecket, V. Mueller, Akademie-Verlag, 1990), on special functions for applied scientists (with A. M. Mathai, Springer, 2008), on the theory and applications of the H-function (with A. M. Mathai, R. K. Saxena, Springer, 2009), and two major review articles on the sun (with A. M. Mathai, Encyclopedia of Planetary Sciences, Chapman and Hall, London, UK, 1997, and Kluwer Academic Publishers, The Netherlands, 2000) and on the structure of the universe (with A. M. Mathai, Encyclopedia of Applied Physics, Vol. 23, Wiley-VCH, New York and Weinheim, Germany, 1998). He is a member of the editorial board of the international journal “Astrophysics and Space Science” and “Earth, Moon, and Planets” (both published by Springer) and STARS (St. Thomas College, Pala, India). He is the (co-)author of more than 250 scientific and technical papers in the fields of astrophysics, mathematics, history of physics, and international cooperation in space science and technology. Since 1988 he has also been with the United Nations Office for Outer Space Affairs, firstly in New York and latterly in Vienna, Austria, since 1993. At the United Nations he spearheaded the development of education curricula in remote sensing and GIS, satellite meteorology and global climate, satellite communications, and space and atmospheric science for the UN-affiliated Regional Centres vii

for Space Science and Technology Education. Since 1991 he is the principal organizer of the United Nations Basic Space Science Initiative and co-editor of 12 volumes of Proceedings that emanated from this initiative. The decadal report on this initiative titled “Developing Basic Space Science World-Wide” was published by Kluwer Academic Publishers, Dordrecht, The Netherlands, in 2004 (co-edited by W. Wamsteker, R. Albrecht, and H. J. Haubold). He is a member of the Centre for Mathematical Sciences (Pala and Trivandrum, India). He is also a member of the German Physical Society, German Mathematical Society, American Mathematical Society, Society for Industrial and Applied Mathematics, American Astronomical Society, History of Science Society, Committee on Space Research, and the International Astronomical Union. He is maintaining websites at neutrino.aquaphoenix.com and www.cmsintl.org.

viii

Biographical Sketch: Dr. Barbara J. Thompson Education B.A., Physics and Mathematics, 1991, University of Pennsylvania Ph.D., Physics, 1996, University of Minnesota

IHY roles Director of Operations, IHY Secretariat IHY Website Editor, IHY Secretariat Member, IHY-USA Organizing Committee Dr. Barbara J. Thompson currently an astrophysicist in the Solar Physics Laboratory at the NASA Goddard Space Flight Center in Greenbelt, Maryland. She has devoted the majority of her solar research to the study of coronal mass ejections and their impact on the heliosphere and near-Earth space. She has also done work on the acceleration of particles in the Earth’s aurora and the Sun’s magnetic structure. She has authored 150 papers on these topics. Born June 17, 1969 in Austin, Texas, she obtained degrees in both physics and mathematics, with a minor in geology, from the University of Pennsylvania in Philadelphia. She received her Ph.D. from the University of Minnesota, with a thesis topic of the acceleration of particles in the Earth’s aurora by waves in the Earth’s magnetosphere. She is a member of the American Astronomical Society, the American Geophysical Union and the International Astronomical Union, and the International Association of Geophysics and Aeronomy (IAGA). She has served as an officer of IAGA and on committees for the AAS and National Science Foundation. Additionally, she was Project Scientist for the Solar Dynamics Observatory and a co-investigator on the Plasma Suprathermal and Ion Composition (PLASTIC) and Sun–Earth Connection Coronal and Heliospheric Investigation (SECCHI) instruments for the Solar–Terrestrial Relations Observatory (STEREO) mission. She has served as the IHY Director of Operations since its inception as well as the website editor. She has helped to plan many IHY workshops and meetings and was the co-leader of IHY’s largest science campaign, the Whole Heliosphere Interval.

ix

Biographical Sketch: Dr. Joseph M. Davila Education B.Sc., Mechanical Engineering, 1972, Lamar University B.Sc., Physics, 1978, University of California – Irvine Ph.D., Astronomy, 1982, University of California – Irvine

IHY Roles Executive Director, IHY Secretariat Chair, IHY International Steering Committee Team Member, IHY-USA Organizing Committee Dr. Joseph Michael Davila is currently an astrophysicist in the Solar Physics Laboratory at the NASA Goddard Space Flight Center in Greenbelt, Maryland. His research interests have included the linear and non-linear theory of hydromagnetic waves, hydromagnetic instabilities due to energetic particle beams, resonance absorption in inhomogeneous plasmas, the acceleration of high-speed wind streams in solar and stellar coronal holes, and plasma heating in closed magnetic structures. He has authored over 150 papers on these subjects. Born December 30, 1948 in Port Arthur, Texas, he earned a bachelor of science degree in mechanical engineering from Lamar University in Beaumont, Texas. He then earned a bachelor of science degree in physics from the University of California, Irvine, in 1978 and a Ph.D. in astronomy from the University of Arizona in 1982. He is a member of the American Astronomical Society, the American Geophysical Union and the International Astronomical Union. He has also published research on the acceleration of cosmic rays, the transport of energetic, particles within the galaxy, the modulation of galactic cosmic rays by the solar wind and the propagation of solar cosmic rays in the interplanetary medium. He was principal investigator for the Solar Extreme-ultraviolet Rocket Telescope and Spectrograph (SERTS), he was the project scientist for the Solar–Terrestrial Relations Observatory (STEREO), and is the lead scientist for Coronagraph-1 (COR1) on the STEREO mission. x

He has served as the IHY executive director from its inception, and has organized many of the IHY conferences and committees. He is now focusing on the transition of IHY programs into the International Space Weather Initiative.

xi

Biographical Sketch: Dr. Natchimukonar Gopalswamy Education B.Sc., Physics, 1975, University of Madras M.Sc., Physics, 1978, University of Madras Ph.D., Plasma Physics, 1982, IIA

IHY roles International Coordinator, IHY Secretariat Team Member, IHY-USA Organizing Committee Dr. Natchimuthukonar Gopalswamy is currently an astrophysicist in the Solar Physics Laboratory of NASA’s Goddard Space Flight Center, Greenbelt, Maryland. As a solar physicist and radio astronomer, Dr. Gopalswamy studies solar variability and its impacts on Earth. He is a co-investigator of the Solar Terrestrial Relations Observatory (STEREO) mission. Over his career to date, he has authored or coauthored more than 300 research papers. Born February 15, 1954 in Chandrapuram, Tamil Nadu, India, he received his B.Sc. and M.Sc. degrees in physics from the University of Madras (1975 and 1977). He received his Ph.D. in plasma physics from the Indian Institute of Astrophysics in Bangalore (1982), followed by a post-doctoral training at the University of Maryland, College Park (1985–1987). He is a member of the American Astronomical Society, the American Geophysical Union and the International Astronomical Union. He promotes international cooperation in space science, serving as the International Coordinator for the IHY 2007 program. He has organized IHY scientific activities in collaboration with international scientific organizations such as the International Astronomical Union (IAU), the Scientific Committee on Solar Terrestrial Physics (SCOSTEP), and the International Association of Geomagnetism and Aeronomy (IAGA). He serves as a member of the SCOSTEP Bureau, representing IAU. As international coordinator for IHY since its inception, he has helped to organize many IHY workshops and meetings. He has been a major driver behind the IHY national programs and the U.N. Basic Space Science instrument development program.

xii

Table of contents

Table of contents Preface: Putting the “I” in IHY. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . v

1 IHY Overview . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1 Looking back on IHY: a statement from the IHY Secretariat . . . . . . . . . . . . 1 1.1 IHY’s foundation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2 1.2 IHY activities: Science, Observatory Development, Outreach and History . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5 1.3 Schedule and legacy plans . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7 1.4 The International Space Weather Initiative (ISWI) . . . . . . . . . . . . . . 10

2 Leadership, Coordination & International Programs . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 11 2.1 2.2 2.3 2.4

Organizational structure . . . . . . . . . . . . . . . . . . . . . . . IHY Secretariat . . . . . . . . . . . . . . . . . . . . . . . . . . . . . The International Advisory and Steering Committees . Regional and national leadership and coordination. . . .

. . . .

. . . .

.. .. .. ..

. . . .

.. .. .. ..

. . . .

. . . .

. . 11 . . 11 . . 12 . . 14

3 Science: Universal Heliophysical Processes and Coordinated Investigation Programmes (CIPs) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 15 3.1 3.2 3.3 3.4

Universal Processes: the foundation of heliophysics . . . Scientific disciplines and the Universal Processes . . . . . Science campaigns and CIPs . . . . . . . . . . . . . . . . . . . International science coordination. . . . . . . . . . . . . . . .

. . . .

. . . .

.. .. .. ..

. . . .

.. .. .. ..

. . . .

. . . .

. . 15 . . 18 . . 19 . . 23

4 IHY/UNBSS Observatory Development Program . . . . 49 4.1 4.2 4.3

Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 49 The U.N. Workshops on Basic Space Science . . . . . . . . . . . . . . . . . . 51 Instrument programs and status . . . . . . . . . . . . . . . . . . . . . . . . . . . . 55 xiii

Table of contents

5 Education and Public Outreach . . . . . . . . . . . . . . . . . . . 87 5.1 5.2 5.3 5.4 5.5 5.6 5.7

Organizational structure . . . . . . . . . . . . . . . . . . . . . . . . . . . Forums: meetings, special sessions, and planning discussions Public events and exhibitions . . . . . . . . . . . . . . . . . . . . . . . Scientific research programs . . . . . . . . . . . . . . . . . . . . . . . . IHY schools and teacher training . . . . . . . . . . . . . . . . . . . . Web and Internet resources . . . . . . . . . . . . . . . . . . . . . . . . Multilingual and multicultural resources . . . . . . . . . . . . . . .

. . . . . . .

.. .. .. .. .. .. ..

. . . . . . .

.. .. .. .. .. .. ..

. 89 . 89 . 91 101 105 115 116

6 “IGY Gold” History initiative . . . . . . . . . . . . . . . . . . . . . 119 6.1 6.2 6.3

Goals . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 119 The IGY “Gold” Club . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 119 Historical commemoration events . . . . . . . . . . . . . . . . . . . . . . . . . . 121

7 IHY National and Regional Committee Reports . . . 125 7.1 7.2 7.3 7.4 7.5 7.6 7.7 7.8

Africa . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Eastern Asia and the Pacific . . . . . . . . . . . . . . . . . . . . Eastern Europe and Central Asia . . . . . . . . . . . . . . . . Balkan, Black Sea and Caspian Sea Regional Network . Western Europe . . . . . . . . . . . . . . . . . . . . . . . . . . . . Latin America and the Caribbean. . . . . . . . . . . . . . . . North America . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Western Asia . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

. . . . . . . .

.. .. .. .. .. .. .. ..

. . . . . . . .

. . . . . . . .

.. .. .. .. .. .. .. ..

. . . . . . . .

.. .. .. .. .. .. .. ..

125 151 177 182 212 267 274 288

Appendix I IHY Committees and Team Leaders . . . . . . 303 Appendix II United Nations Basic Space Science Workshops and Projects . . . . . . . . . . . . . . . 314 Appendix III IHY Publications . . . . . . . . . . . . . . . . . . . . . . 321 1 2 3 4 5 xiv

“Sun and Geosphere” Journal . . . . U.N. Publications and Resources. . Special Issues . . . . . . . . . . . . . . . . Heliophysics textbooks . . . . . . . . . IHY/COST296 Calendar . . . . . . .

. . . . .

. . . . .

.. .. .. .. ..

. . . . .

.. .. .. .. ..

. . . . .

. . . . .

.. .. .. .. ..

. . . . .

. . . . .

.. .. .. .. ..

. . . . .

. . . . .

.. .. .. .. ..

. . . . .

. . . . .

.. .. .. .. ..

. . . . .

.. .. .. .. ..

321 321 323 327 327

Table of contents

Appendix IV IHY Events, Conferences and Seminars . . . . . . . . . . . . . . . . . . . . . . . . . . . . 328 Appendix V IHY and the International Science Years . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 339 1 2

Brief history of the IGY . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 339 The Celimontana Declaration: IHY and the other International Science Years . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 342

Acknowledgments . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 349 Index . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 351 List of figures . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 361

xv

1 IHY Overview

1 IHY Overview

“Space is a part of the world’s cultural heritage. It has inspired generations of artists, poets, scientists and musicians. Throughout history, societies have admired and searched for meaning in the same night sky.” “Indeed, space exploration can help bring cultures together. Manned space missions today are rarely top-secret national projects. Much more common are international crews, with members from a variety of backgrounds. Crews live together in cramped and challenging conditions for months, sharing experiences, customs and, above all, the enthusiasm for space that brought them together in the first place. Their missions capture the imaginations not only of their native lands, but of people around the world.” “Space is also helping us to address some of today’s most urgent problems. Space technology has produced tools that are transforming weather forecasting, environmental protection, humanitarian assistance, education, medicine, agriculture and a wide range of other activities. And, of course, a fascination with space leads many young people to pursue careers in science and technology, helping developing countries in particular to build up their human resources, improve their technological base and enhance their prospects for development.” – U.N. Secretary – General Kofi Annan, on the occasion of World Space Week, 2001 Heliophysical: A broadening of the concept “geophysical,” extending the connections from the Earth to the Sun & interplanetary space. On the 50th anniversary of the International Geophysical Year, the IHY activities will build on the success of IGY 1957 by continuing its legacy of system-wide studies of the extended heliophysical domain.

Looking back on IHY: a statement from the IHY Secretariat The International Heliophysical Year began as a vague concept in late 1999. Over the next few years a series of grassroots community workshops were held, 1

1 IHY Overview

and the IHY began to take shape. In these workshops the concept of Universal Processes was born, and the definition of this new word “heliophysics,” coined to imply a parallelism with geophysics, began to take shape. Also four main thrusts of scientific research, observatory development, history, and outreach were articulated. With this basic organizational structure, the work of planning began. First starting with a few, but then involving more and more space scientists from many countries around the world. Eventually there would be planning committees in nearly 90 nations involving the efforts of thousands of scientists. In March 2007 the IHY was officially opened, and what a success it has been! A total of 65 Coordinated Investigation Programs were initiated for the IHY. Each program involved a team of scientists working together on problems of mutual interest. The distributed instrument program facilitated the deployment of a wide range of instrument arrays all over the world, and in places that were thought to be unreachable. Eclipses in Tunisia and Libyan Arab Jamahiriya opened the door for scientific collaboration, eventually leading to instrument installations in these countries. More than 150 new instruments were installed in Africa, South America, and Asia. These installations will provide a tangible and lasting legacy for the IHY. Outreach programs brought heliophysics into the public eye, with public talks, exhibitions, and a worldwide observatory “Open Doors” day. A number of teacher workshops were organized to distribute newly translated teaching materials to educators, and the IHY Schools program developed new curricula in heliophysics. The IHY Gold history program awarded more than 300 certificates to honor the participation of scientists in the IGY fifty years ago, organized workshops in India, Japan and the USA focusing on IGY history, and sponsored retrospective lectures at a number of meetings. None of these accomplishments would have been possible without the support of funding agencies, scientific organizations and scientists around the world who saw a need, and answered the call. We thank them for their determination, vision, perseverance and friendship.

1.1. IHY’s foundation 1.1.1. IHY’s heritage In 1957–1958 a program of international research, inspired by the International Polar Years of 1882 and 1932, was organized as the International Geophysical 2

1 IHY Overview

Year (IGY) to study global phenomena of the Earth and geospace. The IGY involved about 60,000 scientists from 66 nations, working at thousands of stations from pole to pole to obtain simultaneous, global observations on Earth and in space. There had never been anything like it before. The International Heliophysical Year was inspired by the 50th Anniversary of the International Geophysical Year (IGY) and 50 years of space exploration. IHY builds on the successes of the International Geophysical Year and the previous International Polar Years. We now extend our global studies out into the heliosphere and incorporate the drivers of geophysical change into the global system. As we approach the “new frontier” of the heliopause and interstellar space, our heritage clearly extends back to previous International Years (see Figure 1 and Appendix V). The efforts of the past half-century have brought us significant scientific advances, global scientific communication, and an extensive suite of spacecraft and observatories, which some call our “Great Observatory.” As we extend the reach of human exploration and prepare for humanity’s first encounter with interstellar space, we have expanded our concept of “geophysics” to embrace other planets, interplanetary space, and the Sun itself. The establishment of this new

Uranus Asteroid Belt

Earth

Neptune

Venus

Saturn

Mercury Mars Pluto Jupiter

Fig. 1. The extension of the concept of “geophysical” into “heliophysical”. The tradition of international science years began almost 125 years ago with the first international scientific studies of global processes of polar processes in 1882–1883. A second International Polar Year (IPY) was organized in 1932, but a worldwide economic depression curtailed many of the planned activities. IGY in 1957 was an unprecedented success on many levels. IHY continues the legacy of these previous events, extending global synoptic studies and global interconnected processes to the rest of the heliosphere.

3

1 IHY Overview

science, heliophysics, is the primary goal of IHY: a system-wide understanding of the entire interconnected heliophysical system.

1.1.2. IHY’s goals and objectives Prior to the launch of IHY, an international planning committee, consisting of scientists from around the globe, launched a series of discussions and meetings to establish the principles of IHY and the means by which we would be able to lay the foundation for the new science of heliophysics. It was determined that the efforts of IHY should encompass three primary objectives: *

*

*

Advancing our Understanding of the Fundamental Heliophysical Processes that Govern the Sun, Earth and Heliosphere. Continuing the tradition of international research and advancing the legacy on the 50th anniversary of the International Geophysical Year. Demonstrating the Beauty, Relevance and Significance of Space and Earth Science to the World.

IHY’s priorities are set via its three primary objectives. The first objective, “Advancing our Understanding of the Fundamental Heliophysical Processes that Govern the Sun, Earth and Heliosphere” focuses on our scientific activities, involving an international community of scientists spanning all of the heliophysical disciplines. The second objective, “Continuing the tradition of international research and advancing the legacy on the 50th anniversary of the International Geophysical Year” refers to our commitment to preserving the history and legacy of the IGY through our many scientific research programs, the deployment of new instrumentation worldwide, and our cooperation with other IGY anniversary programs. The third objective, “Demonstrating the Beauty, Relevance and Significance of Space and Earth Science to the World” reminds us of the many applications of heliophysics that are relevant to our existence on earth, and the tremendous opportunity for outreach and education. From these objectives we derive the six goals of IHY, each corresponding to a unique opportunity afforded by the IHY programs: 1. Develop the basic science of heliophysics through cross-disciplinary studies of universal processes. 2. Determine the response of terrestrial and planetary magnetospheres and atmospheres to external drivers. 4

1 IHY Overview

3. Promote research on the Sun–heliosphere system outward to the local interstellar medium – the new frontier. 4. Foster international scientific cooperation in the study of heliophysical phenomena now and in the future. 5. Preserve the history and legacy of the IGY on its 50th anniversary. 6. Communicate unique IHY results to the scientific community and the general public.

1.2. IHY activities: Science, Observatory Development, Outreach and History IHY is an integrated program consisting of many diverse activities that are coordinated on an international level to achieve all of the above goals. Because many of the IHY activities correspond to more than one IHY goal, it became clear that their ideal organization would be based on the nature of the effort. As a result, the International Heliophysical Year Program has four main components: Science, Observatory Development, History and Outreach (Figure 2). The four components of IHY are related to the goals of IHY as follows: Science: IHY’s scientific activities are organized via Coordinated Investigation Programmes (CIPs). The CIPs span all the disciplines throughout heliophysics, and coordinate observations and analysis involving scientists and instrumentation around the world. Using the data resulting from the CIPs, we drive towards a more complete understanding of the universal processes that govern the Sun, Earth, planets and heliosphere. Section 3 of this document contains a more thorough description of the science activities and CIP coordination. Observatory Development: This effort is dedicated to the establishment of observatories and instrument arrays that greatly expands our knowledge of global

Goals 1 – 4 Goals 3 – 4 Goal 5 Goal 6 Fig. 2. The four programmatic components of IHY, and their relationship to the six Goals of IHY. There is a strong overlap between each of the components, indicated in the diagram at right.

5

1 IHY Overview

heliophysical processes, with the added benefit of increasing the viability of space science research and education in developing nations and regions that traditionally have not been active in space research. Fifteen instrument programs, led by scientists around the world, have resulted in new and exciting ionospheric, geomagnetic, and solar measurements. Central to this effort are the United Nations Basic Space Science (UNBSS) workshops, which were dedicated from 2005–2009 to IHY instrument development and data analysis. This joint U.N./IHY developing nations program, described in Sect. 4, targets activities which stimulate Space and Earth Science activities at institutions around the globe. History: IHY is also dedicated to preserving the history and legacy of IGY 1957. Capitalizing on its 50th anniversary, the IGY Gold History Program seeks to identify and recognize planners of and participants in the first IGY, preserve memoirs, articles, photographs, and all items of historical significance for the IGY, make these items available to historians, researchers, etc., spread awareness of the history of geophysics, and plan a series of commemorative special events and “reunions.” These activities are described in Sect. 6 of this document. Outreach: There have been unique opportunities for expanding the education and awareness of Space and Earth Sciences during IHY. As a result, the education programs form a cornerstone of our international initiative. The IHY outreach program focuses on the availability of multilingual materials, so that people from all nations are able to learn about IHY. The IHY Schools Program has given students from around the world an opportunity to attend courses on heliophysics and learn from internationally recognized experts in the field. These efforts are described in Sect. 5 of this document. Although each of the above items has a unique function, it is clear that the coordination of these activities allows us to successfully implement and maximize the impact of each of the components. For example, the Education and Public Outreach component, when integrated with the science campaigns, observatory development, and history initiatives, is able to reach a greater audience and have a larger impact. Similarly, as we establish a greater presence for Space and Earth Sciences in developing nations and underrepresented areas, we also assist the local researchers establish education and outreach initiatives through our international educational programs. Stronger research programs mean stronger universities, which allow the development of graduate and undergraduate programs, which are key factors in encouraging youth to become interested in the exciting field of heliophysics. 6

1 IHY Overview

1.3. Schedule and legacy plans The IHY Opening Ceremony was held on February 19, 2007 in conjunction with the United Nations Science and Technical Subcommittee meeting in Vienna, Austria. A special presentation on IHY plans and activities was made during the Subcommittee session, along with statements of support from the following participating IHY nations: Canada, China, Germany, Greece, Hungary, India, Italy, Japan, Malaysia, Nigeria, Republic of Korea and the United States. Following the subcommittee meeting, U.N. delegates and IHY participants from around the world came together at the Opening Ceremony to formally announce the commencement of the International Heliophysical Year (Figure 3). The Opening Ceremony was chaired by Dr. Joseph M. Davila, the Executive Director of IHY. It was followed by an international planning workshop hosted by the Vienna Academy of Sciences on February 20, 2007. A special IHY exhibit was on display in the United Nations Rotunda throughout the week, featuring over 50 displays from participating IHY nations and programs around the world. As part of this exhibit, two exciting new items were premiered: the

Fig. 3. The “SunWorks” art exhibit premiered at the IHY Opening Ceremony in Vienna, Austria. The exhibit featured sculptures, paintings, and photos from artists around the world.

7

1 IHY Overview

“SunWorks” collection of original Sun-themed artwork from around the world, and four special artistic posters commissioned by IHY representing the IHY’s science activities. The IHY Closing Ceremony will transpire at the United Nations in Vienna on February 18, 2009. Representatives from all of the IHY regions will be present for the celebration. IHY would not have been successful had it not been for the efforts of its science and outreach leaders, who initiated planning activities all over the globe. Hundreds of local, regional and international planning conferences and meetings laid the foundation for IHY. While international conferences serve to connect researchers around the world, workshops focusing on the local scale enabled individual organizations and institutions to develop unique IHY programs that suit their own goals and challenges. It is the activities and programs developed by these individual organizations and institutions that form the “building blocks” of the IHY. Therefore, the IHY’s international planning activities have focused on the establishment of the four main components of IHY (Science, Observatory Development, History and Outreach) and on the integration of the individual IHY regions and nations to maximize success on all levels. The true measure of IHY’s success is not its activities in 2007–2009, but the lasting impact IHY has on heliophysics science and education. IHY is part of the legacy of the International Geophysical Year; 50 years after the program ended, the IGY is still having a significant impact on the scientific community. Just as the planning stage was the key to the successful launch and implementation of IHY, we require a dedicated legacy effort to ensure that the impact of IHY continues. The legacy plan involves three steps: 1. determining whether a particular IHY program will continue to have a significant impact on heliophysics science and/or education if supported beyond 2009, 2. identifying a partner organization or creating a legacy organizational structure that will be able to house that activity, and 3. working with the organization to transfer the program’s knowledge and management from the IHY Secretariat to this new organization. For many IHY programs that were partnerships with other organizations, the legacy plan is to transfer the program to that partner organization. The IHY science collaborations with ICESTAR and CAWSES, for example, will continue to grow under the aegis of these organizations. Many IHY outreach activities, such as Sun–Earth Day and Yuri’s Night, are ongoing activities that 8

1 IHY Overview

will continue their collaboration with individual IHY institutions. The IGY Gold Program will continue to be supported, on a less formal level, by the IHY Secretariat. The Observatory Development program, however, requires the most support over the upcoming decades. It will continue as part of the United Nations Basic Space Science program, but UNBSS requires the continued support of the instrumenters and partner institutions. As a result, a core “IHY Africa” planning group will continue beyond 2009, focusing its efforts on the scientific collaborations and educational activities in regions that will benefit from continued attention. The following is a brief summary of the IHY timeline of activities. A more complete listing of IHY events is included in Appendix IV. 2001–2003: Establishment of IHY Secretariat; establishment of the main elements of the IHY program; initialization of planning activities on all continents. 2004: National and Regional coordination meetings begin to take place; the four essential components of IHY are defined; synergy/coordination discussions with professional organizations; establishment of CIP structure; launch of the IHY UNBSS and IGY Gold History Programs. 2005: Continuation of national and regional coordination meetings; synthesis and coordination from regional to international; precursor activities for each ofthe four main components continue to happen; instrument deployment begins and CIPs proposed by individual community members begin to form the fabric of the IHY science campaigns. 2006: Focus on the implementation of the four main IHY components and on the integration of national and local activities with the international IHY community; prototyping year, particularly for numerous CIPs and outreach activities that serve as trailblazers and/or testbeds. 2007–2008: IHY is launched on March 1, 2007 as an integrated international program. Science, Observatory Development, Outreach and History activities occur around the globe, and the efforts of each individual component and region are multiplied in impact by their coordination with the worldwide effort. 2009–2010: IHY officially ends in February 2009, but many activities continue. Results of the IHY CIPs and science campaigns are analyzed in a wide range of workshops and analysis activities; Observatory Development continues through IHY UNBSS legacy programs; Outreach activities incor9

1 IHY Overview

porate major scientific results and breakthroughs. Legacy transition efforts begin, wherein active IHY programs are transferred from IHY central organization to IHY partner programs. Central to the legacy efforts is the International Space Weather Initiative, described next.

1.4. The International Space Weather Initiative (ISWI) To build on the many advances of the IHY, a new United Nations initiative will be launched: the International Space Weather Initiative (ISWI). The purpose of this effort would be to continue to encourage existing and new scientific collaborations, and begin the process of making the data from the new IHY arrays utilized as part of international space weather alert systems. A special planning meeting will take place during the IHY Closing Ceremony, and a new 3-year work plan will be proposed as an international space weather research program to continue the instrument deployment and operations around the world that was begun during the IHY.

10

2 Leadership, Coordination & International Programs

2 Leadership, Coordination & International Programs

2.1. Organizational structure The IHY program’s organizational structure was devised to balance the priorities and influence of the international coordination teams, the working groups, the individual national IHY programs, and the supporting international scientific bodies and consortia. Figure 1 illustrates how these facets are related; the Steering Committee, International Advisory Committee and Secretariat, respectively, are charged with the guidance, execution, and coordination of IHY’s international activities. Local IHY activities – that is, activities and coordination within a particular region or nation – are represented in the lower portion of the organization chart in Figure 1. Each of the (currently 192) United Nations member states belong to one of the IHY international regions: Africa, Eastern Asia and the Pacific, Eastern Europe and Central Asia, Latin America, North America, Western Asia and Western Europe. The internationally coordinated activities, represented on the right side of the organization chart, are grouped by the four IHY components, described in Sects. 3–6 of this document.

2.2. IHY Secretariat The IHY Secretariat is responsible for the support of IHY committees and international activities. The Secretariat also maintains the IHY website, provides resources for IHY activities, and is responsible for communication within and outside of the participating community. The IHY Secretariat consists of the following: *

* *

Chair of the IHY Steering Committee, who also functions as the Executive Director of the IHY Secretariat International Coordinator Director of Operations

11

2 Leadership, Coordination & International Programs

IHY Activities International Steering Committee International Advisory Committee

Secretariat

E. Europe & Central Asia

E. Asia & Pacific

Africa

Science

Observatory Development

Latin America

History

Outreach North America

Western Asia

Western Europe

National Committees and Activities

Fig. 1. IHY organizational structure.

* * * * * * *

Director of the U.N. Basic Space Science Observatory Development Program Coordinated Investigation Programme (CIP) Coordinator Education and Outreach Coordinator International Advisory Committee Chair “IGY Gold” History Committee Chair Newsletter Editor Website Designer and Editor

The individuals who have filled these many roles are located at various research institutions around the world, drawing support from a wide range of international bodies. A list of the people who have served in these positions is included in Appendix I.

2.3. The International Advisory and Steering Committees As mentioned previously, the guidance, execution, and coordination of IHY international activities are performed by the International Advisory Committee, Steering Committee, and Secretariat, respectively. The membership of the International Advisory Committee was chosen to balance geographical distribution, 12

2 Leadership, Coordination & International Programs

scientific disciplines, and representation from organizations and supporting programs. The International Advisory Committee advises the IHY team on issues of international coordination, planning, and connectivity with international scientific organizations, national bodies, and related activities. This group serves as a consultant body to help optimize the relationship between the goals and efforts of IHY and other international groups and activities. The IHY Steering Committee has the responsibility of ensuring the implementation of the recommendations of the International Advisory Committee, as well as overseeing the operations within IHY. The IHY International Steering Committee is comprised of representatives from each of the seven IHY geographical regions and scientists spanning all of the subdisciplines of heliophysics. The responsibilities of the International Steering Committee include the prioritization of IHY resources and activities, providing guidance and monitoring the progress of the IHY working groups, and ensuring clear communication between the IHY teams, scientific organizations, and constituent bodies. The membership of both of these committees is given in Appendix I.

Fig. 2. There were IHY activities in most of the world’s countries, and many chose to form national organizing committees to stimulate local IHY activities. Nations with IHY national programs are shown in color.

13

2 Leadership, Coordination & International Programs

2.4. Regional and national leadership and coordination There are 78 nations with IHY national committees (see Figure 2), and there are IHY contacts in most of the remaining United Nations member states. The national activities are coordinated within their respective IHY region (Africa, Eastern Asia and the Pacific, Eastern Europe and Central Asia, Latin America, North America, Western Asia and Western Europe). An additional network called the “Balkan, Black Sea and Caspian Sea Regional Network” was formed, which consisted of nations from both the Eastern and Western European regions. In this document, this additional network is included with the Eastern European region. Members from each of the regions are each represented on the IHY Steering Committee. Formal coordination between the regions is handled by the Steering Committee. However, the IHY workshops and planning meetings have served as the primary means of coordination and integration between the regional and national programs. It was at the meetings that the leaders could discuss their priorities and resources, and determine the optimal approach and balance between local and international efforts. Brief summaries of the IHY activities for each of the IHY regions, along with reports for individual nations are given in Sect. 7.

14

3 Science: Universal Heliophysical Processes and CIPs

3 Science: Universal Heliophysical Processes and Coordinated Investigation Programmes (CIPs)

With the phenomenal improvement of ground- and space-based observations since the International Geophysical Year in 1957, the opportunity to observe heliophysical processes has never been better. Today, ground-based observatories routinely observe most domains of heliophysics, often using local measurements to form a global picture. Observatories in space now provide data from locations and regimes that have only recently become accessible, with drastically improved resolution and range, and large-scale computer modelling has made it possible to assimilate and couple these diverse observational inputs, enabling cross-disciplinary studies which transcend traditional boundaries in space physics. It is now widely recognized that much of the space physics of the solar system proceeds through a set of Universal Heliophysical Processes, i.e. magnetic reconnection, particle acceleration, plasma wave generation and propagation, etc. These processes occur in the atmosphere of the Sun, the Earth, and other planets; in the interplanetary medium; and in the outer reaches of the heliosphere where the solar wind meets the interstellar medium. By facilitating research on these Universal Processes across the many heliophysical regimes that serve as independent sampling sites, we are able to gain insight into these driving forces at a fundamental level.

3.1. Universal Processes: the foundation of heliophysics The structure of the Universe is determined primarily by the interplay of gravity which is dominant in condensed objects, and the magnetic force which is dominant in the rarefied medium connecting the Sun and planets, among other realms. Each of these forces order the matter into a set of characteristic structures, each with the ability to store and release energy in response to changes in the external environment (Figure 1). For the most part, the storage and release of energy proceeds through a number of Universal Processes. The coordinated study 15

3 Science: Universal Heliophysical Processes and CIPs

Fig. 1. The energy stored in magnetic structures can be released as kinetic energy (upper left), energetic particles (upper right), waves (lower left), or heating (lower right). Here “B” denotes magnetic field and “E” denotes electric field.

of these processes in different settings provides a deeper understanding of the underlying physics governing Universal Processes in geo- and astrophysics. Magnetic reconnection is one of the best examples of a Universal Process in heliophysics. Reconnection is also observed in the magnetosphere of Earth, particularly in the magnetopause and magnetotail, and the signatures of reconnection are detected throughout the solar wind and it is probable that it will be observed at other planets as well. The energy is released as energetic particles, flows, waves, and plasma heating. Universal Processes are not confined to the ionized plasma component in the Solar System. The Earth’s ionosphere is the boundary between the neutral atmosphere and space. Energy between these two components is exchanged through this boundary. One process by which this energy exchange takes place 16

3 Science: Universal Heliophysical Processes and CIPs

is through atmospheric gravity waves. Gravity waves are excited in the neutral atmosphere by thunderstorms, mountain ranges, and other processes. These waves propagate upward from their point of origin steepening as they propagate. Eventually these waves become nonlinear and “break” like ocean waves on a beach, depositing their energy in the ionosphere–mesosphere, providing a potentially important coupling between the troposphere where climatic effects are evident and the magnetosphere. Figure 2 shows several images of gravity waves in both Earth’s and Mars’ atmospheres. The potential importance of these processes for energy transfer has only recently been recognized, and much additional work remains to establish the significance of the Universal Process of gravity wave propagation on the structure of Earth, Mars, and other planetary atmospheres. The Universal Processes were adopted during the IHY United States Planning Workshop in April 2004, refined in subsequent years, and are described in detail in a new textbook series. Three next textbooks in Heliophysics are created as part of the LWS Heliophysics Summer School 2007–2009, one for each year (see “Publications” Appendix III). A general list of the types of Universal Heliophysical Processes is as follows: Creation & Annihilation of Magnetic Fields Reconnection Dynamos Diffusion Dissipation

Generation of Penetrating Radiation Galactic Cosmic Rays Solar Energetic Particles Anomalous Cosmic Rays Radiation Belts

Couplings of the Sun, Heliosphere, Galactic Environment & Planetary Climate Planetary Dynamo Stellar Dynamos Radiative Couplings Electromagnetic Couplings

Magnetic coupling Non-Local (Non-Contact) Flow-Object Cross-Scale Neutral-Plasma Dusty Plasmas

Explosive Energy Conversions Solar (Stellar) Flares CMEs Substorms Bursty Bulk Flows

Spontaneous Generation of Structures & Transients Flux Ropes-Filaments Current Sheets Cellular Structures Turbulence

The field of comparative aeronomy is leading heliophysics in the examination of Universal Processes, by seeking commonalities in the observations of planets and moons. For example, aurorae (Figure 3) have been observed on Earth, Saturn, and Jupiter, Ganymede, as well as Jovian auroral “footprints” from Io, Ganymede and Europa. The formation of aurorae is observed to be the universal response of a magnetized body in the solar wind. This phenomenon involves several Universal Processes, spanning all of the categories listed above. The cross-disciplinary study 17

3 Science: Universal Heliophysical Processes and CIPs

Fig. 2. Gravity waves in Earth's atmosphere (upper left panel) transfer energy from the troposphere to the ionosphere–mesosphere. Similar waves seen on Mars by the Mars Global Surveyor Mission (lower left and right panels) may couple the lower and upper Martian atmosphere.

Fig. 3. Aurorae on Saturn (left), Jupiter (center left), Earth (center right), and on Ganymede (right) are manifestations of universal physical processes at work in the solar system.

of these processes increases our sample size, treating the whole of heliophysics as our laboratory.

3.2. Scientific disciplines and the Universal Processes The International Heliophysical Year (IHY) focuses on the cross-disciplinary study of Universal Processes in the solar system, observed in a variety of settings. Studying these Universal Processes together, in diverse environments, and in a comparative way, is leading to new scientific insights. For the majority of current scientific studies in heliophysics, however, comparison of processes at multiple sampling sites is either secondary or nonexistent. Most of our scientific organizations categorize research according to the regime in which the studies occur (e.g. solar, magnetospheric, atmospheric) instead categorizing by the fundamental physics. To facilitate the transition from regime-dominated 18

3 Science: Universal Heliophysical Processes and CIPs

science to a focus on Universal Processes, our Coordinated Investigation Programmes (CIPs) are integrated with respect to more “traditional” categories. The IHY disciplines are: * * * * * * *

Solar Physics Heliosphere and Cosmic Rays Magnetospheres Ionized Atmospheres Neutral Atmospheres Climate Studies Meteors/Meteoroids/Dust

Each discipline has one or two scientists who serve as Discipline Coordinators, who review and coordinate the CIPs within their discipline, and work with the other Discipline Coordinators to determine each CIP’s relationship to the Universal Processes described above. A detailed description of the CIP process follows in the next section.

3.3. Science campaigns and CIPs 3.3.1. Infrastructure Three broad imperatives underlay the science coordination approach taken by IHY: first, that it be decentralized, driven by grassroots science interests without a central authority to direct the science; second, that it be a low bureaucracy approach that provided the maximum benefit with the minimum of formal overhead; third, that it should be cross-disciplinary and facilitate investigation of Universal Processes and help researchers to make use of scientific resources with which they were not familiar. The Coordinated Investigation Programme (CIP) mechanism was developed to match these requirements. CIPs are the fundamental building blocks of IHY science and provide the primary mechanism for identifying a science activity as contributing to IHY and for linking those activities together. The model for a CIP was the SOHO Joint Observing Programme (JOP) but with the conscious replacement of “observing” with “investigation” to emphasize that non-observational science activities including theory, modelling and retrospective data analysis were equally welcome. The result was a process that gave open access – anyone could propose a CIP and details of all CIPs are public; and which preserved the autonomy of the activities described in any CIP – the proposer retains control and the IHY infrastructure acts to facilitate and advertise the 19

3 Science: Universal Heliophysical Processes and CIPs

Fig. 4. “How CIPs work” schematic.

proposed activities. The CIP process is illustrated in Figure 4. The top level of the figure denotes an individual researcher, accessing the IHY CIP system via the Internet. Any researcher could propose a CIP designed to address a scientific topic according to expertise and available resources. The second level of Figure 4 illustrates the CIP application and archival process. When a CIP proposal is submitted it is logged and the researcher receives confirmation that the CIP has been placed in the digital archive. CIP descriptions can also be modified, under the control of the original proposer. Notifications of new or updated proposals are also sent to the Discipline Coordinators, who review all CIP proposals and support cooperation and collaboration between related CIPs. An example of how CIPs were clustered in this way is shown in Figure 5. Coordinating the CIPs provides access to a wider range of data that can be assembled and analysed 20

3 Science: Universal Heliophysical Processes and CIPs

Heliosphere/Cosmic Rays

CMEs 3-D Structure of EUV CMEs in the inner corona

lonized atmospheres

CIP 7

Barbara J. Thompson Website Investigating Coronal Filament Cavities

Neutral atmospheres

CIP 21

S. Gibson Website

Climate

IHY Science

Solar

Filaments

CIP 23

Formation and Evolution of Filaments Sarah Gibson Filament activation and its relation to CMEs

Meteors/Meteoroids/Dust

CIP 51

Holly Gilbert Website Study of CMEs/ICMEs Using SOHO/Ulysses Data

Magnetospheres

CIP 71

Cristiana Dumitrache Website

Other

Other

Fig. 5. Example of CIP browser showing CIPs concerned with Solar Filaments in detail.

more efficiently. The discipline coordinators will optimize the schedule of these CIPs to maximize scientific benefit and minimize the strain on needed resources. The final stage of the CIP process occurs months to years later, as the researchers involved in various CIPs participate in one of many workshops to review the outputs of the IHY. This is the process by which the CIPs, organized according to the separate disciplines, are brought into the general paradigm of Universal Processes. A series of cross-disciplinary topical Universal Process workshops, some of are will be through “virtual” Internet communication, will present and discuss the scientific results of the IHY campaigns.

3.3.2. Range and distribution of CIP activities A total of 65 CIPs were submitted with many spanning multiple disciplines, with the numbers in each discipline being: Heliosphere, 29; Solar, 24; Magnetospheres, 34; Ionized Atmospheres, 24; Neutral Atmospheres, 11; Climate, 4; Meteors/ Meteoroids/IPD, 2. They can all be explored online using an online browser tool at http://ihy2007.org.uk/CIP_browser.shtm; an illustration of this browser in use is shown in Figure 5, which shows the details of those CIPs relating to solar filaments expanded as an example. Each red arrow is a link to a web page, those labelled “CIP n” to the CIP details and those labelled “Website” to a pertinent external website. Participation in CIPs has been genuinely multinational with involvement from more than 45 nations in CIPs, either in proposing them or by involvement in their 21

3 Science: Universal Heliophysical Processes and CIPs Participation in the Coordinated Investigation Programme, by state Region

Proposing states

Participating states

Africa

South Africa (5)

Algeria, Cape Verde, Côte d’Ivoire, Egypt, Ethiopia, Libyan Arab Jamahiriya, Morocco, Nigeria, Tunisia

Asia

China (2), India (4), Japan (6)

Republic of Korea, Malaysia, United Arab Emirates

Europe

Armenia, Austria (3), Bulgaria, Czech Republic (2), Finland (6), France, Germany (4), Hungary (4), Ireland, Italy (12), Norway (3), Poland, Romania (2), Russian Federation (6), Slovakia, Spain, Sweden (2), Switzerland, United Kingdom (9), Ukraine (2)

North America

Canada (6), Mexico (2), United States (22)

Costa Rica

South America

Brazil (5)

Argentina, Chile, Peru

Oceania

Australia (2), Indonesia

implementation, spanning all continents. The table above summarizes this, showing the number of CIPs proposed, or jointly proposed, by each country and also those nations involved in CIP implementation. The geographical spread includes Antarctica, an important location for studying geospace, with 12 CIPs incorporating research and data taken from the Antarctic continent. Several broad groupings of CIPs can be identified, indicating clusters of interest in research questions or methods of enquiry. Examples of these include: *

*

Comparative Aeronomy: CIPs such as the “Universality of Auroral Structure” CIP v#3 are spearheading the Universal Processes effort for IHY. CIP #3 takes advantage of our ability to study auroral processes on multiple planets and moons to assess the magnetic environment/energetic-plasma/atmosphere interaction and assess the commonality of auroral manifestations across the heliosphere. Cosmic Rays: Fourteen CIPs are concerned with the study of cosmic rays in the heliosphere. They range across studies of the generation of cosmic rays both in the heliosheath and from the Sun, their transport and modulation through the heliosphere, and their impact on the terrestrial ionosphere. The collaboration of this group of CIPs included organizing a workshop in Bad Honnef, Germany in

22

3 Science: Universal Heliophysical Processes and CIPs

*

*

*

May 2007 covering a wide range of heliophysics but with a particular focus on the interplanetary magnetic field and modulation of Cosmic Ray fluxes. Solar Filaments: Five CIPs were focused on the study of solar filaments including their formation, structure, evolution and their links with Coronal Mass Ejections (CMEs). This cluster of CIPs was instrumental in setting up the most extensive campaign of the IHY science programme – the Whole Heliosphere Interval (WHI). CME Initiation and Propagation: A group of seven CIPs are aimed at the study of the origin of CMEs and their propagation outward from the Sun through the heliosphere to impact Earth, the other planets and spacecraft distributed throughout the solar system. These CIPs constituted another major component of the WHI campaign, making use of data from spacecraft including SoHO, Ulysses, Venus-Express and ACE, together with ground-based observations of the impact of CMEs on the terrestrial magnetosphere and ionosphere. Incoherent Scatter Radars: Five CIPs made use of the global network of Incoherent Scatter Radars. These instruments are few in number, with fewer than ten worldwide, but provide unique multi-parameter diagnostics of the ionosphere and how its behaviour is driven by coupling to the solar wind. The EISCAT Svalbard Radar ran an unprecedented and essentially continuous yearlong operation to support IHY and the IPY from March 2007.

3.4. International science coordination Many organizations played a fundamental role in coordinating IHY scientific activities. There were IHY special sessions at meetings all around the world, and each IHY workshop and conference would not have been possible without support from research agencies and sponsoring organizations. The United Nations Office of Outer Space Affairs provided the basis for the observatory development programme and many of the scientific collaborations associated with that programme. The programmes that have generously provided support for IHY are too numerous to mention. However, we mention three scientific organizations that have played a significant role in IHY’s coordination.

3.4.1. International Astronomical Union The International Astronomical Union deserves special recognition due to its central role in IHY’s scientific activities. David Webb is the IAU’s representative to the IHY, and an IAU Working Group on IHY, chaired by Nat Gopalswamy, has pursued research, collaboration and conference opportunities through the 23

3 Science: Universal Heliophysical Processes and CIPs

IAU. The IAU IHY activities were first discussed at the 2006 IAU General Assembly in Prague, Czech Republic. “Astronomy for the Developing World”, featured a subsession on IHY, and IAU also hosted an international coordination meeting for IHY leaders. The first meeting of the IAU Working Group on IHY also transpired in 2006, and all IHY regions were represented, to make plans for IAU-based activities. The IAU sent statements of IHY support for each of the United Nations Committee on the Peaceful Uses of Space (COPUOS) meetings, and updates on IAU/IHY collaboration were regularly published in the IAU Bulletin and the IHY Newsletter. IAU sponsored IHY’s first conference dedicated to Universal Processes, “IAU Symposium 257: Universal Heliophysical Processes” September 15–19, 2008 in Ioannina, Greece. The conference’s unique format consisted primarily of invited presentations that covered all aspects of heliophysics, allowing researchers to discuss the comparative physics underlying the Universal Processes. At the next IAU General Assembly in Rio de Janiero 2009, there will be a 1.5day special Joint Discussion titled “IHY Global Campaign – the Whole Heliosphere Interval”. The Scientific Organizing Committee consists of IHY scientists from nine different nations, and will highlight the activities of IHY’s largest scientific research campaign. There will also be a special session on the “International Year of Astronomy 2009”, which will provide an opportunity to discuss the transition of IHY activities into the IYA.

3.4.2. The Whole Heliosphere Interval: a global campaign celebrating IHY and our great observatory network http://ihy2007.org/WHI The Whole Heliosphere Interval (WHI) is an internationally coordinated observing and modelling effort to characterize the three-dimensional interconnected solar-heliospheric-planetary system. The heart of the WHI campaign is the study of the interconnected 3-D heliophysical domain, from the interior of the Sun, to the Earth, outer planets, and into interstellar space. Fifty years after the IGY, we 24

3 Science: Universal Heliophysical Processes and CIPs

have observations of the outer reaches of the heliosphere, and we are poised to make great advances in our understanding of our extended heliophysical domain and our relationship with interstellar space. WHI takes full advantage of the 50 years of scientific progress of IGY by coordinating state-ofthe-art models and observations to address the entire interconnected heliophysical system. The WHI observing campaign focused on the 3-D solar structure from solar Carrington Rotation 2068, which ran from March 20 to April 16, 2008. Observations and models of the outer heliosphere and planetary impacts extend beyond those dates as necessary; for example, the solar wind transit time to outer planets can take months. WHI corresponds to several CIPs that focus on multi-spacecraft observations, modelling, and Sun–Earth heliospheric structure. WHI occurred during solar minimum, optimizing our ability to characterize the 3-D heliosphere and trace the structure to the outer limits of the heliosphere. Hundreds of scientists have performed observations and models, which were first discussed at the “WHI Data and Modelling Assessment Workshop” in Boulder, Colorado August 25–29, 2008. A special session on WHI happened at the December 15–19, 2008 American Geophysical Union Meeting, and the WHI Science Workshop is being planned for 2009.

3.4.3. ICESTAR: IHY’s connection to the International Polar Year http://www.scar-icestar.org Interhemispheric Conjugacy Effects in Solar-Terrestrial and Aeronomy Research (ICESTAR) is a Scientific Research Programme endorsed by the Scientific Committee of Antarctic Research (SCAR). According to its name, the ICESTAR community is interested in the Sun–Earth linkage processes with the special emphasis on interhemispheric comparison studies. The programme lasts for 5 years and it started in 2005. IHY together with ICESTAR coordinated an IPY core project (Cluster 63) under the title “Heliosphere impact on geospace”. This initiative includes 29 25

3 Science: Universal Heliophysical Processes and CIPs

international consortia, and it links into several IHY CIPs. These groups conduct research under three main themes: (i) Coupling processes between the different atmospheric layers and their connection with solar activity; (ii) Energy and mass exchange between the ionosphere and the magnetospher and (iii) Interhemispheric similarities and asymmetries in geospace phenomena. The IPY Cluster 63 community runs a large body of instrumentation in both the Arctic and the Antarctic. Many institutes have recently installed new instruments in the polar regions to significantly improve the spatial coverage and resolution and to provide pairs of geomagnetically conjugate observations from both the hemispheres. ICESTAR and IHY have had complementary roles in the IPY Cluster 63 activities: IHY has arranged overarching synoptic observation campaigns and provided systems and assessment processes in order to facilitate the harvesting of interdisciplinary observations. ICESTAR has led the efforts in establishing Virtual Observatories (VOs) for various geospace observations. The Gaia VO for auroral precipitation data and VGMO from magnetic field data are examples of these coordination activities. As scientific output roughly 80 peer-reviewed articles with clear connection to Cluster 63 activities have been published during the period January 2007–June 2008. The following lists all of the IHY Coordinated Investigation Programmes (CIPs). For a more complete summary of the IHY CIPs, please see Sect. 3. CIP 1 Programme title: Coronal mass ejection studies: development of algorithms for CMEs Lead proposer: Professor Richard A. Harrison, Space Science and Technology Department, Rutherford Appleton Laboratory, UK Other proposers: Chris Davis, Danielle Bewsher, Rutherford Appleton Laboratory, UK; Andrew Breen, University of Wales Aberystwyth, UK; David Webb, Hanscom Air Force Base Research Lab, USA Scientific disciplines: Solar; Heliosphere/cosmic rays Scientific synopsis: Using a combination of white light wide-angle imaging of the heliosphere and EUV monitoring of the corona, the aim of this project is to develop specific tools for the prediction of CME onsets and CME arrival at Earth using several spacecraft platforms. 26

3 Science: Universal Heliophysical Processes and CIPs

CIP 2 Programme title: Real-time global ionosphere Lead proposer: Tim Fuller-Rowell, Space Weather Prediction Center, USA Scientific discipline: Ionized atmospheres Scientific synopsis: Characterizing the global ionospheric variability. CIP 3 Programme title: Universality of auroral structure Lead proposer: Dr. Anil Bhardwaj, Space Physics Laboratory; Vikram Sarabhai Space Centre, India Other proposer: Marina Galand, Imperial College London, UK Scientific discipline: Planetary magnetospheres; Ionized atmospheres; Neutral atmospheres Scientific synopsis: Assessing the magnetic environment, energetic plasma, and atmosphere interaction: how does the magnetic environment interact with the ionosphere? Assess the commonality across auroral manifestations in the heliosphere. CIP 4 Programme title: Global plasmaspheric dynamics Lead proposer: Ian Mann, Department of Physics, University of Alberta, Canada Scientific disciplines: Planetary magnetospheres; Ionized atmospheres; Neutral atmospheres Scientific synopsis: Characterize plasmaspheric erosion and refilling. CIP 5 Programme title: State of the LISM at the heliospheric boundary and inside Lead proposer: Prof. Eberhard Moebius, Space Science Center, University of New Hampshire, USA Other proposers: Prof. Hans R. Mueller, University of New Hampshire, USA Scientific discipline: Heliosphere/cosmic rays Scientific synopsis: How does the interstellar gas in the inner heliosphere change with the solar cycle? What are the defining features of neutral gas–plasma interaction? CIP 6 Programme title: Environment termination shock and the heliosheath Lead proposer: Matthew E. Hill, Applied Physics Laboratory, Johns Hopkins University, USA 27

3 Science: Universal Heliophysical Processes and CIPs

Other proposers: Mike Gruntman, University of Southern California, USA; William Kurth, University of Iowa, USA Scientific discipline: Heliosphere/cosmic rays Scientific synopsis: (A) What is the nature of the heliosphere near the TS? (B) What are the properties of the shock? (C) What is the nature of heliospheric turbulence? CIP 7 Programme title: 3-D structure of EUV CMEs in the inner corona Lead proposer: Barbara J. Thompson, NASA GSFC, USA Scientific disciplines: Solar; Heliosphere/cosmic rays Scientific synopsis: We will conduct a comprehensive campaign to take advantage of the multiple instruments observing CMEs in the corona and inner heliosphere to determine the relationship between the structure represented by the EUV images (SOHO/EIT, TRACE, PROBA2/SWAP, STEREO/SECCHI) and the coronal white-light structures (Mauna Loa MkIV, SOHO/LASCO, STEREO/SECCHI). We will map the EUV signatures (dimmings, filaments, expanding loops, EIT waves) into the coronal structures as represented by the coronagraphs, with the goal of understanding more clearly the structure and manifestations of CMEs in the low corona. CIP 8 Programme title: Mid- and high-latitude ionospheric–magnetospheric observations Lead proposer: Dr. Pierre Cilliers, Hermanus Magnetic Observatory, South Africa Other proposers: Prof. Harm Moraal, North-West University, South Africa; Dr. Cathryn Mitchell, University of Bath, Bath, UK; Dr. Lucilla Alfonsi, INGV, Rome, Italy Scientific disciplines: Planetary magnetospheres; Ionized atmospheres; Neutral atmospheres Scientific synopsis: To better understand magnetospheric and ionospheric variability in the time range from seconds to days and longer and their links to the solar wind and magnetospheric phenomena. CIP 9 Programme title: Modelling variable cosmic ray fluxes in the dynamic heliosphere, magnetosphere, and atmosphere as well as their imprints on Earth Lead proposers: Klaus Scherer, Institut fuer Theoretische Physik, Germany; Marius Potgieter, School of Physics, North West University, South Africa 28

3 Science: Universal Heliophysical Processes and CIPs

Other proposers: Juerg Beer, EAWAG, Switzerland; Hans-Joerg Fahr, University of Bonn, Germany; Stefan Ferreira, North West University, South Africa; Horst Fichtner, University of Bochum, Germany; Bernd Heber, University of Kiel, Germany; Josef Masarik, Komensky University, Slovakia Scientific disciplines: Planetary magnetospheres; Heliosphere/cosmic rays; Ionized atmospheres; Neutral atmospheres Scientific synopsis: The aim of this proposal is to make a synoptic model for the production rates of cosmogenic isotopes, taking into account the cosmic ray transport and its long-term variability, the dynamics of the heliosphere and its variation with interstellar changes, and the transport of cosmic rays through the magnetosphere and atmosphere, to describe the effects on the Earth’s environment. CIP 10 Programme title: Empirical model of ring current distributions Lead proposer: Anna Milillo, INAF/IFSI, Italy Other proposer: Stefano Orsini, INAF/IFSI, Italy Scientific discipline: Planetary magnetospheres Scientific synopsis: The first aim of this project is to obtain from local ion measurements of the global evolution of the ring current plasma distributions during quite time as well as geomagnetic storm development (real-time global ring current). The second aim is to obtain zero order global plasma distributions by knowing the solar wind parameters at Earth (short-time forecast). CIP 11 Programme title: Three-dimensional view of inner heliosphere and predicting the arrivals of coronal mass ejections Lead proposer: P. K. Manoharan, Radio Astronomy Centre, Tata Institute of Fundamental Research, India Other proposers: M. Kojima, Kyushu University, Japan; B. V. Jackson, University of California, San Diego, USA; J. A. Gonzalez-Esparza, Instituto de Geofisica, UNAM, Mexico; A. Breen, University of Wales Aberystwyth, UK; Xizhen Zhang, University of Colorado, USA Scientific disciplines: Solar; Heliosphere/cosmic rays; Solar and heliosphere Scientific synopsis: Coordinated IPS and SMEI observations of the heliosphere to study the three-dimensional view of the solar wind flow and turbulent plasma associated with CMEs; the aim is to predict the arrival of CME at 1 AU. CIP 12 Programme title: SOHO-Ulysses coordinated studies during the two extended quadratures and the alignment of 2007–2008 29

3 Science: Universal Heliophysical Processes and CIPs

Lead proposers: G. Poletto, Arcetri Astrophysical Observatory, Italy; S. Suess, NASA Marshall Space Flight Center, USA Scientific disciplines: Solar; Heliosphere/cosmic rays Scientific synopsis: When Ulysses is 90 around the Sun from Earth (in ‘quadrature’), the same plasma observed remotely from, e.g., SOHO can later be observed in situ. Ulysses will be in near-quadrature for 5 months in winter 2007 and again in winter 2008. We will use the quadratures to analyze physical parameters (density, temperature, composition, . . .) in outflows and transients. In summer 2007, Ulysses passes through a radial alignment with Earth, during which we will analyze composition and transport of energetic particles. CIP 13 Programme title: High energy processes and dynamics of the low solar atmosphere during explosive events Lead proposer: Jean-Pierre Raulin, Universidade Presbiteriana Mackenzie, Brazil Other proposers: V. S. Makhmutov, E. Correia, P. Kaufmann, C. Mandrini, W. Bandeira, M. Luoni Scientific discipline: Solar Scientific synopsis: To bring observational clues on the total number of accelerated particles during the impulsive phase of solar flares, to better constraint existing acceleration models. From the gradual development of solar flares we address the dynamics of the low solar atmosphere. Finally we are interested exploring the relationship between the launch of CMEs and the activity close to the solar disk as seen at high frequency radio wavelengths. CIP 14 Programme title: Ionospheric effects of the solar activity variations, solar flares, lightnings and energetic particle precipitations. Lead proposers: J.-P. Raulin, E. Correia, V. S. Makhmutov, Universidade Presbiteriana Mackenzie, Brazil Other proposers: A. A. Pacini, W. M. Carvalho, M. Aparecido Scientific disciplines: Ionized atmospheres; Neutral atmospheres Scientific synopsis: This project is concerned with the physical sources of the disturbances in the Earth’s ionosphere at different time and space scales and their influence on the characteristics of very low frequency wave propagation. CIP 15 Programme title: Influence of Sun and other cosmic factors on environment of the Earth 30

3 Science: Universal Heliophysical Processes and CIPs

Lead proposer: Dr. Saumitra Mukherjee, School of Environmental Sciences, India Scientific disciplines: Solar; Heliosphere/cosmic rays; Planetary magnetospheres; Ionized atmospheres; Neutral atmospheres; Climate Scientific synopsis: It has been observed that earth directed coronal mass ejection from the Sun along with the cosmic influence has the potential to change the environment of the earth temporarily. The changes in the electron flux and planetary indices have been observed before the occurrence of earthquake, tsunami, sudden snowfall, heat wave and cloudburst. Cosmic influence of the sun needed to be observed on continuous basis on the Sun as well as on the earth and other planets of the solar system. CIP 16 Programme title: Investigation of the high energy particle precipitation in the lower and middle atmosphere in the southern hemisphere magnetic anomaly (SHMA) Lead proposer: Dr. Luis Eduardo Antunes Vieira, Max Planck Institute for Solar System Research, Germany Scientific disciplines: Solar; Heliosphere/cosmic rays; Planetary magnetospheres; Neutral atmospheres; Climate Scientific synopsis: The main goal of the program proposed is the investigation of the cosmic rays modulation of the cloud properties and net radiative flux in the southern hemisphere magnetic anomaly region. CIP 17 Programme title: Dynamics of the magnetosphere Lead proposer: Prof. Umberto Villante, Physics Department, University of L’Aquila, Italy Other proposers: Dr. Marcello De Lauretis, Dr. Patrizia Francia, Dr. Massimo Vellante, University of L’Aquila, Italy; Dr. Roberto Bruno, Dr. Raffaella D’Amicis, INAF-IFSI, Italy Scientific disciplines: Planetary magnetospheres; Ionized atmospheres Scientific synopsis: We use measurements of the geomagnetic field variations at both high and low latitudes for a continuous monitoring of the dynamical processes of the Earth’s magnetosphere as well as a ground support to space missions. CIP 18 Programme title: Spatial and temporal TEC characterization of the ionosphere in the South Atlantic magnetic anomaly Lead proposer: Emilia Correia, Universidade Presbiteriana Mackenzie, Brazil Other proposers: Edvaldo S. Fonseca Jr., PTR/USP; J. F. G. Monico, Paulo O. Camargo, UNESP/Pres.Pru.; Sonia M. A. Costa, Luiz P. S. Fortes, IBGE; 31

3 Science: Universal Heliophysical Processes and CIPs

Eurico R. de Paula, Ivan J. Kantor, INPE; Jean Pierre Raulin, Pierre Kaufmann, CRAAM/UPM; Jose H. Fernandez, UNITAU; Paulo R. Fagundes, UNIVAP; Leonardo C. Oliveira, IME, Brazil Scientific discipline: Ionized atmospheres Scientific synopsis: The goal of this work is to characterize the spatial and temporal variations of TEC surrounding the South Atlantic magnetic anomaly (SAMA); during quiet and magnetically disturbed periods. The TEC will be obtained from GPS measurements realized by the Brazilian continuous GPS network. CIP 19 Programme title: Transport of mass and energy across the magnetopause during periods of northward IMF and their effects on the high latitude ionosphere Lead proposer: M. F. Marcucci, INAF–IFSI, Italy Other proposers: E. Amata, D. Ambrosino, M. B. Bavassano Cattaneo, M. Candidi, G. Consolini, I. Coco, S. Massetti Scientific disciplines: Planetary magnetospheres; Ionized atmospheres Scientific synopsis: We propose to study the plasma and energy transport processes from the solar wind to the magnetosphere during periods of northward IMF. For that purpose, we will use space borne and ground based data available during IPY. The main emphasis will be put on: CLUSTER, for the high latitude magnetopause, DOUBLE STAR for the equatorial magnetopause, SuperDARN for the polar and auroral ionosphere. CIP 20 Programme title: Space weather in solar system (SWISS) Lead proposer: Dr. Larisa Trichtchenko, NRCanada/ISES, Geomagnetic Laboratory, Canada Other proposers: Dr. Xingqiu Yuan, Geomagnetic Laboratory, Canada; Dr. Konstantin Kabin and Dr. Robert Rankin, University of Alberta, Canada; Dr. Hans de Sterk and Mr. P. Stechlinski, University of Waterloo, Canada; Ms. Zdenka Smith, Dr. Tom Detman, Dr. Murray Dryer, NOAA/Space Weather Prediction Center, USA; Prof. Charles Deehr and Dr. Wei Sun, Geophysical Institute, University of Alaska, USA; Dr. Ghee Fry, Exploration Physics International Inc., USA; Dr. Devrie Intriligator, Carmel Research Center, USA; Prof. Shi Tsan Wu, Dr. Chin-Chun Wu, University of Alabama, USA; Dr. Susan McKenna-Lawlor, Space Technology Ireland Ltd., Ireland; Mr. Brian Choi, Carleton University, Canada Scientific disciplines: Solar; Heliosphere/cosmic rays; Planetary magnetospheres Scientific synopsis: To provide information on current, past and future (forecasted) space weather conditions in the Solar system, useful for planned 32

3 Science: Universal Heliophysical Processes and CIPs

and current space missions and to provide boundary conditions for more detailed models and case studies. To provide a common frame for numerical models of solar wind-planetary magnetospheres interaction during quiet and disturbed times. CIP 21 Programme title: Investigating coronal filament cavities Lead proposer: S. Gibson, NCAR High Altitude Observatory, USA Other proposers: J. Burkepile, G. de Toma, NCAR High Altitude Observatory, USA Scientific discipline: Solar Scientific synopsis: We will gather 3D, multiwavelength observations to constrain forward models of the three-dimensional density, temperature, and magnetic structure of coronal cavities. We will investigate the relationship of cavities to filaments and filament channels. We will also observe the evolution of cavities that erupt as CMEs. CIP 22 Programme title: CME initiation, evolution, and propagation throughout heliosphere Lead proposer: John Raymond, Harvard-Smithsonian Center for Astrophysics, USA Other Proposer: L. Strachan Harvard-Smithsonian Center for Astrophysics, USA Scientific discipline: Solar Scientific synopsis: Comprehensive understanding of CMEs. How do CMEs evolve as they propagate from the Sun through the heliosphere? How are CME shocks formed and what is their relationship to SEPs? CIP 23 Programme title: Formation and evolution of filaments Lead proposer: Sarah Gibson, NCAR High Altitude Observatory, USA Scientific discipline: Solar Scientific synopsis: Understand filaments in the context of the global solar magnetic field. How do filaments form and how do they evolve in time? CIP 24 Programme title: Effective temperature of the quiet sun Lead proposer: P. Fox, NCAR High Altitude Observatory, USA Other proposer: David Rust, JHU/APL, USA Scientific discipline: Solar 33

3 Science: Universal Heliophysical Processes and CIPs

Scientific synopsis: Determine the long term changes in Total Solar Irradiance at Solar Minimum – What are the connections between irradiance, solar radius, and surface magnetic field? What are the effects of coronal holes and chromospheric network on full disk TSI? What is the effective temperature of the Sun (mean and variance)? Are there slowly changing, large-scale variations in the distribution of the sources of TSI on the solar disk? What causes TSI variations that do not correlate with magnetic features? CIP 25 Programme title: ISPAM Lead proposer: A. P. van Eyken, EISCAT Scientific Association, Sweden Other proposers: The Incoherent Scatter Working Group of URSI Scientific discipline: Ionized atmospheres Scientific synopsis: ISPAM is a coordinating activity between the high-latitude incoherent scatter radars to provide extensive ionospheric monitoring during the IPY. The resulting data set is widely applicable to studies of solar–terrestrial interactions, atmospheric tides and waves, and modelling (including now- and forecasting) activities. CIP 26 Programme title: Investigating electromagnetic couplings and plasma environment change in geospace using MAGDAS magnetometer network Lead proposer: Kiyohumi Yumoto, Space Environment Research Center, Kyushu University, Japan Scientific discipline: Planetary magnetospheres Scientific synopsis: (1) By monitoring the global three-dimensional current system, we seek to understand the electromagnetic coupling between high-latitude and Sq current systems. (2) How does the plasma environment change during space storms? (3) How does the polar electric field penetrate into the equatorial ionosphere? CIP 27 Programme title: Cosmic ray tranport/modulation in the 3-D A-negative heliosphere Lead proposer: John W. Bieber, Bartol Research Institute, University of Delaware, USA Other proposers: B. McKibben, Space Science Center, University of New Hampshire, USA Scientific discipline: Heliosphere/cosmic rays 34

3 Science: Universal Heliophysical Processes and CIPs

Scientific synopsis: (A) What is the high energy radiation environment at Earth and in interplanetary space and how does it change over time? (B) What are the causes of GCR modulation? (C) What are the changes of the GCR spectrum? (D) What are the connections between GCRs and climate? (E) How does particle transport work? (F) What is the nature of heliospheric turbulence? CIP 28 Programme title: Evolution of magnetic fields from the Sun’s surface to the heliopause for one solar cycle Lead proposer: N. Schwadron, Boston University, USA Other proposers: C. Smith, Bieber, Bartol Research Institute, University of Delaware, USA Scientific discipline: Heliosphere/cosmic rays Scientific synopsis: (A) What is the 3D structure of the magnetic field in the quiet heliosphere? (B) What are the heliospheric signatures of the global magnetic field reversal in each 11-year cycle? (C) How do the photospheric, coronal, and interplanetary magnetic fields relate to each other? (D) What are interplanetary signatures and effects of reconnection? CIP 29 Programme title: Comparative shock study Lead proposer: M. Lee, University of New Hampshire, USA Scientific discipline: Heliosphere/cosmic rays Scientific synopsis: (A) What are the properties of shocks? (B) How do shock properties scale with the shock parameters? (C) How does interplanetary acceleration change with solar cycle? (D) What is the nature of heliospheric turbulence? CIP 30 Programme title: POLARIS: polarization of the red thermospheric line Lead proposer: Jean Lilensten, Laboratoire de Planetologie de Grenoble, France Other proposers: Dr. Joren Moen, F. Sigernes, University of Oslo, Norway; D. Lorentzen, University Centre in Svalbard, Norway; C. Simon, M. Bartholomy, Laboratoire de Planetologie de Grenoble, France; Roland Thissen, Laboratoire de Chimie-Physique, France Scientific disciplines: Ionized atmospheres; Neutral atmospheres Scientific synopsis: Half a century ago was performed the last measurement of the oxygen red line by Duncan (1958) during the International Geophysics Year. This measurement has been since then disputed and never confirmed (Chamberlain 1959). We have now the opportunity to perform again this measurement in Svalbard (Norway), after promising theoretical developments on the polarization of the red line made in France. This project will open, as the International Polar 35

3 Science: Universal Heliophysical Processes and CIPs

Year is drawing near, a new field of investigation allowing a never-done before diagnostic of the upper atmosphere, which will have a direct impact on orbitography computations. Moreover, almost 50 years after the first measurements, it will build a historical tribute to Duncan’s work on the subject. CIP 31 Programme title: Measurements of the elemental composition and energy spectra of the high-energy cosmic rays and the gradient of the Earth’s magnetic field by high-altitude balloon flight around the North Pole Lead proposer: Prof. Konstantin A. Kotelnikov, Fian, Russia Other proposers: Prof. Yury P. Tsvetkov, Prof. N. S. Svirzhevsky, Prof. E. V. Vashenyik, Dr. T. I. Sysoeva, Dr. V. S. Puchkov, Dr. S. V. Filippov Scientific discipline: Heliosphere/cosmic rays Scientific synopsis: Arrangement of the high-altitude balloon flight around the North Pole. Balloon magnetic field measurements in the Earth’s atmosphere with magnetic gradiometer. Measurements of the elemental composition and energy spectra of the high-energy cosmic rays. CIP 32 Programme title: Decameter investigation of the Sun’s activity Lead proposer: Brazhenko Anatoly Ivanovich, Ukraine Scientific discipline: Solar Scientific synopsis: To receive the polarizing characteristics of a sporadic radio emission of the Sun in decameter lengths of waves. CIP 33 Programme title: IASWR – Antarctic space weather reports Lead proposer: Phil Wilkinson, IPS Radio and Space Services, UK Other proposer: Dr. Giorgiano De Franceschi Scientific discipline: Ionized atmospheres Scientific synopsis: The principal outcome of this proposal will be increased awareness of the problems inherent in forecasting the high-latitude ionosphere in a region of sparse observations, such as encountered in the Antarctic. The database created during the period will also form a baseline collection against which later forecasting efforts may be compared. To date, no similar data set is readily available, although the task of making space weather forecasts is a well developed, if not a mature enterprise. CIP 34 Programme title: balloon borne investigation of Earth, atmosphere and space in the polar regions 36

3 Science: Universal Heliophysical Processes and CIPs

Lead proposer: Silvia Masi, Physics Department, University La Sapienza, Italy Other proposers: Paolo de Bernardis, Steven Peterzen, Roberto Ibba, Domenico Spoto, Giovanni Romeo, Kjell Boen, Simona Di Pippo Scientific discipline: Other (stratospheric balloons and related science) Scientific synopsis: Stratospheric Long Duration Balloons facility in the polar regions for earth, atmospheric physics and cosmological studies can answer several open questions in science, and can carry instruments to be tested before a satellite mission is launched. CIP 35 Programme title: Coordinated study on solar wind turbulence during Lead proposers: Roberto Bruno, INAF-IFSI, Italy; Zoltan Voeroes, Space Research Institute, Austrian Academy of Sciences, Austria; Vincenzo Carbone, Universita della Calabria, Dpt. Fisica, Italy Other proposers: R. D’Amicis, A. Mura, A. Milillo, S. Orsini, B. Bavassano, M. Cattaneo, P. Veltri, L. Sorriso-Valvo, T. Zhang, H. Biernat, H. Rucker, W. Baumjohann, D. Jankovicova, P. Kovacs Scientific discipline: Solar; Other (solar wind turbulence) Scientific synopsis: At the end of August 2007, Venus, Earth and Ulysses will be aligned within a few degrees. This unusual event gives the opportunity to attempt a coordinated study on the radial evolution of solar wind turbulence and coronal transients like CMEs between 0.7 and 1.4 AU. CIP 36 Programme title: International network for auroral optical studies of the polar ionosphere (short title: auroral optical network) Lead proposer: Ingrid Sandahl, Swedish Institute of Space Physics, Sweden Other proposers: Dr. Kirsti Kauristie, Finnish Meteorological Institute, Finland; Prof. Takehiko Aso, National Institute of Polar Research, Japan; Dr. Eric Donovan, University of Calgary, Canada; Dr. Stephen Mende, Space Science Laboratory, UC Berkeley, USA; D. D. Vladimir Safargaleev, Polar Geophysical Institute, Russia; Dr. E. M. Blixt, University of Tromso, Norway; Dr. Dag Lorentzen, The University Centre in Svalbard, Norway; Prof. Joran Moen, University of Oslo, Norway; Dr. Mike Kosch, Lancaster University, UK; Dr. Ian McWirther, University College London, UK; Professor Roger Smith, University of Alaska, USA Scientific disciplines: Planetary magnetospheres; Ionized atmospheres; Neutral atmospheres 37

3 Science: Universal Heliophysical Processes and CIPs

Scientific synopsis: The optical aurora is the only visible manifestation of the physical processes occurring in the Earth’s magnetosphere as it responds to the solar wind, the interplanetary magnetic field, and their often dramatic changes. Studies of the optical aurora is an efficient way to learn about both temporal and spatial variations of these processes and is also a powerful tool for monitoring the Sun–Earth interaction. The emissions contain information both about the incident primary particles and about physical and chemical processes occurring locally as the light is produced. The usefulness of ground-based optical measurements is enhanced by the possibility of combining them with information from satellites. CIP 37 Programme title: Interplanetary causes of intense magnetic storms Lead proposer: Walter D. Gonzalez, INPE, Brazil Other proposers: Ezequiel Echer, Alisson Dal Lago, Fernando Guarnieri, Alicia de Gonzalez, Bruce Tsurutani Scientific disciplines: Planetary magnetospheres; Other (interplanetary-magnetosphere coupling) Scientific synopsis: During the IHY it is of interest to perform a study about the interplanetary causes of intense storms (Dst <  100 nT) that may occur. The particular position of this year within the solar cycle (start of the ascending phase?) presents an interesting challenge for this research. We expect that the results of this study will present a helpful material for the identification of solar sources of such storms, which could be performed in collaboration with other participant groups, which will be studying the solar activity during the IHY. CIP 39 Programme title: ULF waves in the magnetosphere Lead proposer: Balazs Heilig, Tihany Geophysical Observatory, Hungary Scientific disciplines: Planetary magnetospheres; Ionized atmospheres Scientific synopsis: (A) Monitoring ionosphere–plasmasphere dynamics at midlatitudes; (B) Monitoring upstream wave related ULF Pc3 pulsations. CIP 40 Programme title: Conjugate study on magnetospheric cusp dynamics Lead proposer: Huigen Yang, Polar Research Institute of China, China Other proposers: Natsuo Sato, National Institute of Polar Research, Japan; Asgeir Brekke, University of Tromso, Norway; Hu Hongqiao, Zhang Beichen, Liu Ruiyuan, Polar Research Institute of China, China 38

3 Science: Universal Heliophysical Processes and CIPs

Scientific disciplines: Planetary magnetospheres; Ionized atmospheres Scientific synopsis: Investigating dynamics of the magnetospheric cusp. (1) Conjugate study of auroras and ionosphere at cusp latitudes. (2) Ground-based observation of signatures of cusp and solar wind–magnetosphere interaction. CIP 41 Programme title: Radio tomographic imaging of the Arctic ionized atmosphere by the International Ionospheric Tomography Community (IITC) Lead proposer: S. Eleri Pryse, University of Wales Aberystwyth, UK Other proposers: H. R. Middleton, L. Kersley, University of Wales Aberystwyth, UK; J. A. Secan, E. J. Fremouw, Northwest Research Associates, USA; G. S. Bust, Applied Research Laboratories, University of Texas, USA; T. Turunen, Sodankyl Geophysical Observatory, University of Oulu, Finland; E. D. Tereshchenko, Polar Geophysical Institute, Russia; V. E. Kunitsyn, M. Lomonosov Moscow State University, Russia Scientific discipline: Ionized atmospheres Scientific synopsis: The project aims to investigate the impact of space weather processes on the terrestrial ionized atmosphere and identify the relative roles of the geophysical processes that influence the large-scale plasma distribution. The basic physics and chemistry of ionization production and loss in the polar regions are understood reasonably well, including effects of large-scale plasma transport and precipitation of charged particles into the atmosphere. However, the actual structure present in any given situation depends on the relative contributions of the various processes and the balance remains an open question that needs to be addressed by experimental observations. CIP 43 Programme title: SMEI and IPS 3D heliospheric analysis comparison with Ulysses and other NASA spacecraft Lead proposer: Bernard V. Jackson, University of California, San Diego, USA Other proposers: David Webb, Hanscom Air Force Base Research Lab, USA; Masayoshi Kojima, Kyushu University, Japan Scientific disciplines: Solar; Planetary magnetospheres; Heliosphere/cosmic rays Scientific synopsis: We wish to compare the Solar Mass Ejection Imager (SMEI) 3D data reconstruction analyses (density) and with interplanetary scintillation (IPS) data (to measure velocities) during specific time intervals to compare with the Ulysses spacecraft, and other NASA spacecraft instrumentation (i.e., Mars Global Surveyor magnetospheric measurements at Mars) and perhaps use future Faraday rotation observational data to provide global 3D heliospheric reconstructions of density, velocity and magnetic field in comparison with existing NASA spacecraft resources. 39

3 Science: Universal Heliophysical Processes and CIPs

CIP 44 Programme title: Cosmic rays in the heliosphere Lead proposer: Marius Potgieter, Unit for Space Physics, North-West University, South Africa Other proposers: Prof. Adri Burger, Dr. Stefan Ferreira, Mr. Jasper Snyman, Mr. Donald Ngobeni Scientific discipline: Heliosphere/cosmic rays Scientific synopsis: Numerical and theoretical modelling of the transport, acceleration and modulation of galactic and anomalous cosmic rays in the heliosphere. CIP 45 Programme title: Imaging the density structure of the inner magnetosphere Lead proposer: Dr. Endawoke Yizengaw, UCLA, USA Scientific disciplines: Planetary magnetospheres; Ionized atmospheres Scientific synopsis: Imaging the structure of electron density profiles of the innermagnetosphere region to address the following puzzling issues. These include: (1) What is the relative plasmaspheric and ionospheric contribution to the ground based GPS derived TEC changes? Does the plasmaspheric percentage contribution vary as a function of local-time, latitude, season, and geomagnetic and solar activities? (2) How does the density of the plasmasphere behave as a function of altitude, local-time, latitude, season, and geomagnetic and solar activities? (3) How do the dynamics of refilling and erosion of plasmaspheric density behave as viewed from tomographic images of the topside ionosphere and plasmasphere? Is the field aligned damping of plasma to the lower side ionosphere really responsible for the inside the plasmasphere density depletion? CIP 47 Programme title: VLF and ULF waves and particles Lead proposer: Arthur R. W. Hughes, School of Physics, University of KwaZuluNatal, South Africa Other proposers: Andrew Collier, University of KwaZulu-Natal, South Africa Scientific discipline: Other (Geospace Physics) Scientific synopsis: To establish the connection between geomagnetic Pc5, Pi2 pulsations, VLF waves, magnetic sub-storms and particle precipitation. CIP 48 Programme title: Heavy ion outflow from the dayside ionosphere: multi-point view Lead proposer: Yulia V. Bogdanova, Mullard Space Science Laboratory, University College London, UK 40

3 Science: Universal Heliophysical Processes and CIPs

Other proposers: C. J. Owen, MSSL, UCL, UK; I. McCrea, J. Davies, Rutherford Appleton Laboratory, UK; B. Klecker, MPE Garching, Germany Scientific disciplines: Planetary magnetospheres; Ionized atmospheres Scientific synopsis: The aim of this project is a better understanding of the massloading mechanism of the heavy ions from the ionosphere into the magnetosphere especially during storm-time. The important questions are: (1) Location of the dayside outflow – is it concentrated near the cusp region or evenly distributed over a broad range of MLT? (2) Question of quasi-neutrality in the region with ion outflow. (3) Latitudinal extent of the region with heating of ions at different altitude (ionosphere level and 3–6 RE level) (4) What is the exact mechanism of energy transfer from the solar wind into the ionospheric ion outflow? (5) What are the locations and properties of ion outflow under northward IMF? (6) Where are the ions going to? CIP 49 Programme title: COST296/IHY Lead proposer: Giorgiana De Franceschi, INGV-RM2, Upper Atmosphere Physics Unit, Italy Other proposers: COST296/IHY Coordination Team Members Scientific discipline: Ionized atmospheres Scientific synopsis: Since the 1990s the COST Actions relating to ionospheric physics are particularly useful in creating a critical mass of researchers to increase the knowledge of the ionosphere and its effects on navigation and communication systems. Nowadays COST296 Action (2005–2009) (www. COST296.rl.ac.uk) provides a unique European forum for the progression of such matters. In the IHY frame the idea is to maintain the necessary European cooperation for a multi-instrument monitoring of the middle–upper atmosphere and improving scientific joint efforts to investigate on the interconnection between low, mid- and high-latitude ionosphere. This proposal hopes for an integration of other interested middle–upper atmosphere scientific groups. CIP 51 Programme title: Filament activation and its relation to CMEs Lead proposer: Holly Gilbert, NASA GSFC, USA Other proposers: Terry Kucera, Gary Kilper, NASA GSFC, USA; Rui Liu, Rice University, USA Scientific discipline: Solar Scientific synopsis: We will conduct a comprehensive observational study on filament activation, taking advantage of multiple instruments observing filaments 41

3 Science: Universal Heliophysical Processes and CIPs

in the chromosphere and CMEs in the corona to better understand how this process works and how it is related to CMEs. CIP 53 Programme title: Modelling the magnetosheath flow and magnetopause location in the cusp region Lead proposer: Ermanno Amata, IFSI-INAF, Italy Other proposers: Monio Kartalev, P. S. Dobreva, Maria Federica Marcucci, D. Ambrosino Scientific discipline: Planetary magnetospheres Scientific synopsis: The cusp regions are of great importance for understanding the solar wind influence on the Earth’s environment. One outstanding problem in this respect is to explain the detailed features of the flow and the shape and position of the magnetopause in such regions. The model reproduces the cusp indentation and represents a substantial step ahead with respect to previous ones. Moreover it requires only a usual PC, taking reasonable computational time, promising in this way to be a useful tool for data interpretation. CIP 54 Programme title: Inferring the magnetospheric global potential distribution from SuperDARN data through the IMech numerical model Lead proposer: Monio Kartalev, Bulgarian Academy of Sciences, Bulgaria Other proposers: E. Amata, I. Coco, K. Grigorov, M. F. Marcucci Scientific discipline: Planetary magnetospheres Scientific synopsis: The ionospheric electrodynamics is a key element of the solar wind–Earth interaction and of the global electric circuit directly affecting the biosphere. To address this issue, a new global model has been developed at the Institute of Mechanics (IMech) of the Bulgarian Academy of Sciences, Sofia. This model, unlike previously published ones, includes field-aligned currents between magnetically conjugate points and treats separately the northern and southern ionospheres, without forcing the potentials at conjugate points to be equal. In order for the model to run, it is necessary to feed it with distributions of the polar field aligned current system calculated for both hemispheres, e.g. by the AMIE model, which is based on a large collection of data from various instruments. In this CIP we plan to test the model by using potential distributions obtained from SuperDARN data through the JHUAPL model. CIP 55 Programme title: Ionospheric studies through GPS, ionosonde and AWSOME Lead proposer: Dr. Kamlesh N. Pathak, Department of Physics, S. V. National Institute of Technology, India 42

3 Science: Universal Heliophysical Processes and CIPs

Scientific discipline: Ionized atmospheres Scientific synopsis: The aim of the study is twofold: (1) We are starting postgraduate program in Space Physics where the deployment of various heliospheric instrumentation shall be utilized for hands on experimentation to the students. (2) At Surat which is at 21.16 N and 72.78 E coordinates ionospheric studies are sparse. As the location is just below the anomaly the upper ionospheric observations will throw some light on the characteristics of the ionosphere. Also by the deployment of VLF receiver system like AWSOME a complete ionospheric study capability will be available. CIP 56 Programme title: Research of highest energy solar cosmic rays Lead proposer: A. Chilingarian, Cosmic Ray Division, Armenia Other proposers: G. Karapetyan Scientific discipline: Heliosphere/cosmic rays Scientific synopsis: Available experimental data on the GLEs confirm proton acceleration up to 20 GeV, acceleration to higher energies is not reliably proved. Middle- and high-latitude neutron monitors cannot be used for the reconstruction of the primary energy spectra well above 5 GeV because of very weak fluxes and rather small sizes of the detectors. Along with operation of the AMMM we plan to develop new type world-wide network of particle detectors, measuring neutral and charged fluxes simultaneously and to be installed at middle and low latitudes. New particle detectors will perform monitoring of various species of secondary cosmic rays with different energy thresholds. CIP 57 Programme title: Solar minimum watching with Italian SINERGIES and more Lead proposer: Dr. Marisa Storini, INAF/IFSI-Roma, Italy Other proposers: Researchers from INAF, INFN, INGV, CNR, UNICatania, UNIL’Aquila, UNIPerugia, UNIRm1, UNIRm2, UNIRm3, UNISiena, UNITrieste, UNIUrbino, Italy Scientific disciplines: Solar; Heliosphere/cosmic rays (terrestrial science) Scientific synopsis: We use measurements of the different and complementary ground-based instruments managed by research groups of the Italian Astrophysics Community, together with some in situ data, to characterize the solar–terrestrial system during the current solar activity minimum phase (transition from sunspot cycles 23 to 24) in the period in which there is a null subEarth point on the Sun. 43

3 Science: Universal Heliophysical Processes and CIPs

CIP 58 Programme title: Muon diagnostics of heliosphere and the near-Earth space Lead proposer: D. A. Timashkov, NEVOD, MEPhI, Russia Other proposers: N. S. Barbashina, V. V. Borog, A. N. Dmitrieva, R. P. Kokoulin, K. G. Kompaniets, A. A. Petrukhin, D. A. Room, V. V. Shutenko, I. I. Yashin Scientific disciplines: Heliosphere/cosmic rays; Planetary magnetospheres; Neutral atmospheres Scientific synopsis: High-energy galactic cosmic rays penetrate the Solar system from all directions and bring to the Earth information about various dynamic processes in the heliosphere. Though primary and solar cosmic rays do not arrive to the Earth’s surface, the secondary muons produced in the atmosphere reach the ground level keeping the initial particle direction that allows to “X-raying” the inner structure of heliosphere disturbances and to reveal them from large distances from the Earth. CIP 59 Programme title: Universal and individual properties of solar eruptions and their interplanetary consequences: dimensionless scaling Lead proposer: I. S. Veselovsky, Institute of Nuclear Physics, Moscow State University, Russia Scientific disciplines: Solar; Heliosphere/cosmic rays Scientific synopsis: The aim of this project is the application of dimensionless scaling to the construction of experimentally based conceptual models of solar flares, eruptive prominences, coronal mass ejections and their interplanetary manifestations. CIP 60 Programme title: Influence of space weather on micrometeoroid flux Lead proposer: Dr. Thomas Djamaluddin, National Institute of Aeronautics and Space, Indonesia Scientific disciplines: Solar; Heliosphere/cosmic rays; Meteors/meteoroids/dust Scientific synopsis: Preliminary Studies on meteor flux detected by Meteor Wind Radar (MWR) Serpong (near Jakarta, Indonesia) during 1992–1992 and MWR Kototabang (near Bukittinggi, Indonesia) during 2002–2006 indicate that the flux are affected by ecliptic and solar activity variation. Long-term MWR data from all over the world and in situ dust detector on space facility are expected to infer space weather influence on distribution variation of micrometeoroid in Earth orbit. The next question is whether space weather from solar activities affecting the meteor flux be due to atmospheric or interplanetary mechanism. 44

3 Science: Universal Heliophysical Processes and CIPs

CIP 61 Programme title: Solar–heliospheric sources of energetic particles Lead proposer: Peter Kiraly, KFKI Research Institute for Particle and Nuclear Physics, Hungary Other proposers: Dr. Karoly Kecskemety, KFKI, Hungary Scientific discipline: Solar; Heliosphere/cosmic rays Scientific synopsis: (A) Study of spatial and temporal variations of suprathermal and energetic particle fluxes throughout the heliosphere. (B) Study of anisotropy as a function of flux levels. (C) Time-shifted cross-correlation of particle fluxes for various energies. (D) Quiet-time properties of particle populations, including spectral shape, the existence of stable lower bounds, and the dependence on distance from the Sun. (E) Comparison of particle flux characteristics recently measured by Voyager with those measured in the inner heliosphere. (F) Search for nuclear interaction products in heliospheric suprathermal and energetic particle populations.

CIP 62 Programme title: Polar gateways to heliophysical exploration Lead proposer: John F. Cooper, NASA GSFC, USA Other proposers: Dieter Bilitza, Nan Lal, Robert E. McGuire, John W. Mitchell, Robert E. Streitmatter, Steven J. Sturner, Matthew E. Hill, Thomas P. Armstrong, Robert B. McKibben, John D. Richardson, Rogelio Caballero Lopez, Harm Moraal, Kirsti Kauristie, Brian Fraser, Phil Wilkinson, Martin Friedrich, Glenn W. Sheehan, Werner Singer, Akira Yamamoto, Koji Yoshimura, Tetsuya Yoshida Scientific discipline: Heliosphere/cosmic rays Scientific synopsis: Overall theme: Cosmic ray proton energy flow through the heliosphere to geospace and the polar ionosphere. This investigation addresses the heliospheric flow of cosmic ray energy, mostly in protons, from sources at the Sun, within the heliosphere, and from outside the heliosphere to the geospace environment and into the polar ionospheres. Key questions are (1) the source, loss, and transport processed for cosmic ray protons from tens of keV to GeV and above energies; (2) specification of proton flux spectra averaged over solar cycle time scales for effects on planetary surfaces and atmospheres; (3) specification of the instantaneous and time-averaged spectra for protons in geospace; (4) models for propagation of cosmic ray protons through the geomagnetic field into the polar atmospheric environments; and (5) correlative ground-based measurements for cosmic ray contributions to the polar ionospheres. 45

3 Science: Universal Heliophysical Processes and CIPs

CIP 64 Programme title: VLF remote sensing of the daytime and nighttime lower ionosphere Lead proposer: Umran Inan, Stanford University STAR Laboratory, USA Other proposers: Phil Scherrer, Deborah Scherrer, Morris Cohen, Sheila Bijoor; Stanford University, USA Scientific discipline: Solar; Heliosphere/cosmic rays; Planetary magnetospheres; Ionized atmospheres Scientific synopsis: Using very low frequency (VLF, 3–30 kHz) remote sensing techniques, disturbances in the lower ionosphere can be effectively detected and quantified. Disturbances come from a wide variety of sources, including lightning, magnetospheric electron precipitation, auroral activity, solar flares, solar eclipses and cosmic rays. The goal of this project is to understand the ionospheric effects of these processes on a more global scale, using an array of VLF receivers, known as AWESOME, distributed throughout the planet. CIP 65 Programme title: Meteors in the earth atmosphere and meteoroids in the solar system Lead proposer: Kolomiyets Svitlana V., Meteor Radar Centre, Kharkiv National University of Radioelectronics, Ukraine Scientific disciplines: Heliosphere/cosmic rays; Ionized atmospheres; Climate; Meteors/meteoroids/dust CIP 66 Programme title: Solar variability impact on the middle atmosphere Lead proposer: Victor I. Fomichev, Department of Earth and Space Science and Engineering, York University, Canada Other proposers: Theodore G. Shepherd, Andreas I. Jonsson, Charles McLandress, University of Toronto, Canada; John (Jack) C. McConnell, Stephen R. Beagley, Kirill Semeniuk, York University; Stella M. Melo, Chao Fu, Canadian Space Agency, Canada Scientific disciplines: Neutral atmospheres; Climate Scientific synopsis: Solar variability affects the middle atmosphere through both variations in solar spectral irradiance and particle precipitation (Galactic Cosmic Rays, Aurora, Solar Proton evens). The goal of this project is to model the middle atmosphere response to solar variability and build a hierarchy of different forcing mechanisms. CIP 67 Programme title: Steps of the Bashful Ballerina: global structure of the solar/inner heliospheric magnetic field 46

3 Science: Universal Heliophysical Processes and CIPs

Lead proposer: Kalevi Mursula, Physics Department, University of Oulu, Finland Scientific disciplines: Solar; Heliosphere/cosmic rays Scientific synopsis: Recently, systematic hemispheric and longitudinal differences have been detected in the properties of the heliospheric magnetic field (HMF) and in the heliospheric current sheet (HCS). HCS has been found to be shifted southwards during a few years in the late declining to minimum phase of the solar cycle. This is related to the simultaneous development of a global quadrupole moment in the solar coronal field. It has also been found that the HMF sector structure depicts an interesting flip-flop cycle of about 3.2–3.5 years, in analogy of a similar cycle of solar active longitudes. This CIP concentrates on these and related issues, aiming to obtain new insight using different solar and heliospheric parameters from several data bases. CIP 68 Programme title: Modelling of cosmic ray induced ionization of the atmosphere Lead proposer: Ilya Usoskin, Sodankyla Geophysical Observatory, University of Oulu, Finland Other proposers: Dr. G. A. Kovaltsov, Ioffe Physical-Technical Institute, Russia Scientific disciplines: Heliosphere/cosmic rays; Ionized atmospheres Scientific synopsis: The aim of the proposal is to develop a realistic model of cosmic ray induced ionization of the earth’s atmosphere, that should be valid in the whole range of parameters, from the ground to the upper atmosphere, from polar regions to the equator, and from the solar minimum to maximum. CIP 69 Programme title: Rapid solar wind and its impact on the geomagnetic variability Lead Proposers: Ovidiu Maris, Institute for Space Sciences (ISS), Romania; Crisan Demetrescu, Institute of Geodynamics of the Romanian Academy, Romania Other proposers: Georgeta Maris, Venera Dobrica, Institute of Geodynamics, Romania Scientific disciplines: Solar; Heliosphere/cosmic rays; Planetary magnetospheres Scientific synopsis: (a) Identifying the high-speed streams (HSSs) in solar wind during the 1996–2006 interval; (b) Spectral analysis of the HSS parameters; (c) Geomagnetic variability analysis (using aa, IHV, IDV, Dst indices); (d) Study of the “cause and effect” relationship between HSS and geomagnetic variability; improvement of forecast methods. CIP 71 Programme title: Study of CMEs/ICMEs using SOHO/Ulysses data Lead proposer: Cristiana Dumitrache, Astronomical Institute of Romanian Academy, Romania 47

3 Science: Universal Heliophysical Processes and CIPs

Other proposers: Marilena Mierla, A.I.R.A., Diana Constantin, Iulia Chifu, Oana Chiricuta, Adrian Sabin Popescu, Adrian Oncica, Nedelia Antonia Popescu, Vasile Mioc Scientific disciplines: Solar; Heliosphere/cosmic rays Scientific synopsis: Study of solar sources of CMEs (polar prominences, active regions). Follow-up of CMEs from SOHO to Ulysses or track back of ICMEs from Ulysses to the Sun CIP 72 Programme title: Meteors in the Earth atmosphere and meteoroids in the solar system Lead proposer: Oleg Belkovich, Kasan State University, Zelenodolsk, Russia Other proposers: Dr. Marina Ishmukhametova, Dr. Vladimir Andreev, Nail Suleymanov, Engelhardt Astronomical Observatory, Russia; Students (5), Kazan State University, Zelenodolsk, Russia Scientific discipline: Meteors/meteoroids/dust Scientific synopsis: Application of the modern methods of processing of meteor radar observations made in Kazan, Russia, in the 1960s and 1970s of the last century to find out structures of the main meteor streams (meteoroid flux densities and mass index S as functions of the Solar magnitude). Comparison with results obtained from visual observations. CIP 73 Programme title: Meteors in the Earth atmosphere and meteoroids in the solar system Lead proposer: Prof. Nelly Kulikova, Obninsk State Technical University, Russia Other proposers: Dr. Valentina Tishchenko, Dmitriy Kalinin, Nicolay Polyakov, Students (3); Obninsk State Technical University, RUSSIA; Dr. Valentina Chepurova, Moscow State University, Russia Scientific discipline: Meteors/meteoroids/dust Scientific synopsis: Studies of meteoroid danger on Earth and in space. Investigation of the formation and evolution of meteoroid complexes in comet disintegration by probability methods and stochastic approaches. The criteria of comet stream and flux generality. Development of a computer technology.

48

4 IHY/UNBSS Observatory Development Program

4 IHY/UNBSS Observatory Development Program

4.1. Introduction The purpose of the Observatory Development component of the IHY is to develop activities and facilitate partnerships that stimulate Space and Earth Science activities throughout the world, particularly in developing or undersampled regions, such as the establishment of ground-based instrument arrays and research programs. This includes the deployment of small, inexpensive instruments such as magnetometers, radio antennas, GPS receivers, all-sky cameras, etc. around the world to provide global measurements of ionospheric and heliospheric phenomena. This joint program, a collaboration between the IHY and the United

AGREES AMBER AMMA AWESOME CALLISTO CARISMA GPS-Africa ITNE MAGDAS MUON RENOIR SAVNET SCINDA SEVAN SID

Fig. 1. Map indicating instrument deployments supported as part of the IHY/UNBSS program. Please note that the map does not include the majority of the observatories participating in IHY, only those participating in the instrument development program. Many of the national reports in Sect. 7 contain summaries of observatories that participated in IHY campaigns but are not shown on this map.

49

4 IHY/UNBSS Observatory Development Program

Nations Basic Space Science (UNBSS) Initiative, centers around a series of annual workshops hosted in varying international locations. Fifteen instruments have participated in this activity, and as a result of this program more than 150 new instruments and nearly 300 educational SID instruments (see Sect. 5) have been deployed worldwide, with a significant fraction from Africa. The map in Figure 1 indicates the location of the instruments deployed as part of IHY. The Observatory Development program has focused on facilitating partnerships between instrument providers and instrument host institutions. The lead scientist, or principle investigator (PI) provides instrumentation (or fabrication plans for instruments) for the array; the host country provides the workforce, facilities, and operational support to obtain data with the instrument, typically at a local university. The instrument hosts then participate in research data analysis activities culminating in the UNBSS workshops.

Exemplary Science on a Global Scale: Connecting Local Ionospheric Disturbances to Global Processes Figure 2 shows the effects on the naturally occurring ionospheric emissions caused by an instability process generated at the magnetic equator in addition to a geomagnetic storm. The local structures, seen in the data as depletions in the airglow intensity, are caused by an instability process generated at the magnetic equator. The turbulence within these local structures can disrupt transionospheric communication and navigation signals. The local structure typically drifts from west to east. In this example, simultaneous with the development of this equatorial instability process, a traveling ionospheric disturbance (TID) propagates equatorward from the polar region, launched by energy input in the auroral region due to the onset of a geomagnetic storm. Within this TID are electric fields and neutral winds which can differ significantly from their respective quiet-time values. As the TID passes over Hawaii, the perturbed electric fields and neutral winds affect the observed local structure by both reversing the drift direction to the west and initiating the development of secondary instabilities on the eastern edge of the primary local structure.

50

4 IHY/UNBSS Observatory Development Program

630.0 nm, Feb. 04, 2003 06:59 UT

630.0 nm, Feb. 04, 2003 07:32 UT

630.0 nm, Feb. 04, 2003 08:04 UT

630.0 nm, Feb. 04, 2003 08:28 UT

630.0 nm, Feb.04, 2003 09:01 UT

630.0 nm, Feb. 04, 2003 09:33 UT

630.0 nm, Feb. 04, 2003 09:58 UT

630.0 nm, Feb. 04, 2003 10:30 UT

630.0 nm, Feb. 04, 2003 11:02 UT

630.0 nm, Feb. 04, 2003 11:27 UT

630.0 nm, Feb. 04, 2003 11:59 UT

630.0 nm, Feb. 04, 2003 12:31 UT

26 24 22 20 18 16 ADU

-162 -160 -158 -156 -154 -152

500 83311661500 1833 2166 2500

Fig. 2. A series of images capturing the development of structures, seen as dark regions, associated with an equatorial instability process. These structures are further modified by the passage of a traveling ionospheric disturbance, seen as an enhancement traveling from northeast to southwest, associated with energy input in the auroral region. The images are of the 630.0-nm emission that occurs naturally in the Earth’s ionosphere/thermosphere system and were recorded from the site of the Haleakala Volcano on Maui, Hawaii.

The instabilities introduced by TIDs and other ionospheric phenomena impact our ability to communicate through the ionosphere (e.g. GPS, SATCOM). The lack of ability to predict such phenomena leads to unanticipated transionospheric communications outages that negatively impact everyday aspects of life in the 21st Century. In order to mitigate those outages, we need a global predictive capability. A global capability requires comprehensive and extended observations that can resolve both the fine scale structures as well as the global coupling effects that influence the development, structure, and impact of ionospheric disturbances on transionospheric radio signals.

4.2. The U.N. Workshops on Basic Space Science The United Nations, in cooperation with the European Space Agency, initiated in 1990 the organization of annual Workshops on Basic Space Science through the 51

4 IHY/UNBSS Observatory Development Program

United Nations Office for Outer Space Affairs. These Workshops, focusing on astrophysics and space science, have been held in a variety of locations, balancing the geographical representation of the program activities (for a more complete summary of the Basic Space Science Workshops and projects, please see Appendix II). The participation in these workshops is balanced between scientists from developed nations, scientists from developing nations, and scientists from geographical areas near the site of the workshop. The workshops from 2005 to 2009 have been dedicated to the IHY, and their format has provided an ideal venue to bring instrumenters and potential instrument hosts together. The 2005 IHY/ESA/UNBSS Workshop, which was the first of the U.N. workshops dedicated to IHY, was held in Al-Ain, United Arab Emirates. Highlights of this activity included the first instrumentation deployed as a part of this program and the initiation of many collaborations that resulted in other instrument deployments. The 2009 workshop will be hosted by Republic of Korea.

4.2.1. Brief Summary of the UNBSS/ESA Workshop on the IHY, held in Al-Ain, United Arab Emirates, 20–23 November 2005 The 4-day workshop was hosted by the United Arab Emirates University, under the patronage of H. H. Sheikh Nahayan Mabarak Al-Nahayan, Minister of Education and the Chancellor of the United Arab Emirates University, and on behalf of the United Arab Emirates (UAE) Government. The meeting was coorganized by the Committee on Space Research (COSPAR), the International Astronomical Union (IAU) and the National Astronomical Observatory of Japan (NAOJ) and the Department of Physics at the UAE University. The local organization was also provided by the Department of Physics at UAE University. Workshop participants represented 44 United Nations member states, including a significant portion of North Africa, the IHY-West Asia region, as well as leadership from the remaining six IHY international regions. There were special sessions on IHY instruments and host institutions, as well as IHY science, global scientific initiatives, education programs, astrophysical research in Arab nations, and the 2005 World Year of Physics. Special discussions also included planning for the IHY-Africa initiative, education and outreach activities. The primary achievement of this meeting was the initiation of many IHY UNBSS instrumentation activities, whereby an instrument provider is able to find host sites in other nations to increase the coverage of vital scientific measurements. 52

4 IHY/UNBSS Observatory Development Program

4.2.2. Brief summary of the UNBSS/NASA on the IHY, held in Bangalore, India, 27 November–1 December 2006 The Indian Institute of Astrophysics hosted this 5-day meeting. There were 95 participants from 30 different nations. Presentations were given on IHY science and instrumentation, and there was a special working group session on outreach in India and internationally. This workshop built on the success of the previous year. The instrumentation programs initiated during the first workshop in the UAE were developed and a survey was performed of potential host institutions. Scientists representing the host institutions were invited to participate in the meeting, and much of the discussion centered on the instrumentation programs.

4.2.3. Brief summary of the UNBSS/ESA/NASA/JAXA workshop on the IHY, held in Tokyo, Japan, 18–22 June 2007 The next UNBSS/IHY workshop was held at the National Astronomical Observatory of Japan in Tokyo. Nearly 80 participants from 28 nations participated in this workshop, which focused on the continued support of the instrumentation/ host programs, as well as the development of scientific collaborations and analysis efforts for the new IHY instrument arrays. Special discussions focused on the participation of developing nations in IHY, the operation of new facilities in developing nations (see the BSS “Tripod” below), access to data of the Sun–Earth system from ground-based and space-borne facilities through data archives and virtual observatories.

4.2.4. Brief summary of the UNBSS/ESA/NASA/JAXA workshop, “First Results of the International Heliophysical Year,” held in Sozopol, Bulgaria, 2–6 June 2008 This workshop was held in Sozopol, Bulgaria, hosted by the Solar-Terrestrial Influences Laboratory of the Bulgarian Academy of Sciences on behalf of the Government of Bulgaria. There were three major topics around which the meeting was structured. Two of the topics continued the efforts of previous workshops: “Participation of nations in project development for international heliospheric 53

4 IHY/UNBSS Observatory Development Program

Brief Summary of the IHY-Africa Space Weather Science and Education Workshop held in Addis Ababa, Ethiopia 12–16 November 2007 The annual IHY UNBSS workshops have been extremely successful in stimulating space science instrumentation in developing areas, particularly Africa. A special IHY-Africa focus group identified a need for a workshop to support African research activities and to further develop research partnerships in conjunction with the instrumentation program. In response to this need, more than one hundred international scientists met in Addis Ababa, Ethiopia, in November 2007, for a special IHY workshop focused on Space Weather Science and Education. The meeting was the culmination of more than 2 years of planning, spurred on by the IHY-United Nations Basic Space Science (UNBSS) Initiative to promote African space weather science and further deployment of instrument arrays in developing countries. The IHY-Africa workshop had two overall objectives: *

*

To study space weather science at mid and low latitudes in the African longitude sector. To support African space science and education.

The success of the workshop was greatly assisted by the generous support by several national and international organizations including the National Aeronautics and Space Administration (NASA), National Science Foundation (NSF), European Office of Aerospace Research and Development (EOARD), International Center for Theoretical Physics (ICTP), Air Force Office of Scientific Research (AFOSR), Office of Naval Research (ONR), Air Force Research Laboratory (AFRL), Climate and Weather of the Sun–Earth System (CAWSES), and Committee for Space Research (COSPAR). We were also fortunate that representatives of many of the sponsoring agencies were able to attend the meeting. The science focus was built around three major themes: 1. Ionospheric Irregularities. 2. Ionospheric Total Electron Content. 3. Equatorial Electrodynamics and Plasmasphere/Ionosphere Coupling. The ionospheric irregularities session was an extension to the 1-day SCINDA workshop held on the Sunday preceding the IHY workshop.

54

4 IHY/UNBSS Observatory Development Program

There was also a special GIFT Teacher workshop (see Sect. 5) sponsored by NASA and the Houston Museum of Natural History, as well as an AWESOME educational space weather monitor training session. Another workshop, building on the results of this workshop, is being planned in Zambia in June 2009.

space missions and supporting low-cost ground-based instrument array initiatives for world-wide studies in space science” and “Access to data of the Sun–Earth system from ground-based and space-borne facilities through data archives and virtual observatories.” Due to the success of these two efforts, a third topic could now be raised: “First results of the International Heliophysical Year.” A total of 150 scientists representing 36 different nations participated in this meeting.

4.3. Instrument programs and status Drawing on 17 years of experience, U.N. Basic Space Science Initiative developed the “Tripod” concept, an implementation model for the accelerated establishment of basic space science associated activities in developing nations. The Tripod concept, identified in the very first UNBSS workshop in India in 1991, is described as follows: 1. The availability of research tools of a level where meaningful science can be made, but at a level where the national socio-economical infrastructure can maintain functionality in the university/research laboratory environment, e.g. a small telescope facility or instrument array. 2. Teaching materials allowing basic space science to be introduced at the teaching level of fundamental mathematics, physics, chemistry and astronomy courses in middle and higher education. 3. Application materials for original research in basic space science, such as observing programs or software development. The Tripod concept has been central to the selection of the instrument programs for the IHY. Several initiatives that had reached a mature stage of development were selected for the first phase (2005–2006) of the joint IHY/UNBSS Observatory Development activity. Following the early success of this phase, more instrument programs were added for a total of 15, including GPS and ionospheric networks, magnetometers, radio observatories, and particle and muon detectors. The instrument programs were prioritized 55

4 IHY/UNBSS Observatory Development Program

based on suitability to accomplish the joint goals of the IHY and UNBSS programs: *

*

*

Production of scientifically significant and publishable results pertaining to the objectives of the IHY activities; Identification of activities which can be performed in developing nations (many of which are near the equator); and Costs and technical requirements must be compatible with the resources available in the participating nations. Additionally, the following factors were viewed as desirable:

*

*

*

Legacy Potential: leading to a beneficial relationship for the participants in developing nations. “Tiered” Technology: instruments with several designs corresponding to increasing design complexity. Educational components, including university level (such as the AWESOME SID monitors described in Sect. 5).

The efforts of the IHY activity have focused on finding host sites for the observatories and instruments and assisting in the identification of technical and financial resources. The following sections give summaries of the IHY observatory deployment programs.

4.3.1. IHY UNBSS instrument programs 4.3.1.1. GPS & ionospheric networks 4.3.1.1.1. African GPS Receivers for Equatorial Electrodynamics Studies (AGREES)

PIs: Endawoke Yizengaw and Mark Moldwin, University of California at Los Angeles In looking at a map of the world showing the location of ground-based space physics instrumentation (radars, magnetometers, ionosondes, GPS dual frequency receivers, and lidars), one quickly recognizes Africa’s relative lack of space physics research infrastructure. This has created a gap of global understanding of the physics behind the evolution and formation of plasma irregularities in the equatorial region, which imposes severe limitations on ionospheric and plasmaspheric density modeling efforts. Knowledge of ionospheric and plasmaspheric (inner magnetospheric) density structure is required to create weather dependent 56

4 IHY/UNBSS Observatory Development Program

density model and mitigate the navigation and communication degradation. Understanding the source and loss processes of plasma during magnetically active and quiet periods also requires knowledge of inner magnetospheric density structure. Knowing the topside ionosphere and plasmasphere density structure is also essential for obtaining the density contributions of these regions to the ground based total electron content (TEC), which is a long-standing problem. The question is how do we obtain reliable density structure of the inner-magnetosphere as a function of local time and magnetic activity? The scientific community has been developing and using different means to gather density information on the ionosphere and plasmasphere. This includes: incoherent scatter radar probing, coherent scatter radar observations of under dense electron density irregularities, observations using topside sounders onboard satellites, just mention few. However, they are sparsely located around the globe and unable to provide the global understanding of the inner-magnetospheric density structure and dynamics. The ground- and space-based GPS receivers continuously provide the integrated total electron content (TEC) between the satellite and receiver on the ground, which is one of the most important quantitative characteristics of the ionosphere and plasmasphere. However, the uneven distribution of ground-based GPS receivers hinders our ability to obtain a global understanding of the dynamics and structures of the inner magnetosphere. Although ground-based GPS receivers are located in dense regional arrays, they are primarily only in North America and Europe. In regions like Africa, observations of the inner-magnetosphere are not possible due to lack of ground-based instruments. The density structure over this region has been traditionally estimated by using vast areas of model interpolation. Therefore, to have a complete and global understanding of the electrodynamics of the inner-magnetosphere in a cost effective way, deployment of small instruments, like ground-based GPS receivers, is essential. Therefore, the AGREES (African GPS Receivers for Equatorial Electrodynamics Studies) GPS receivers network in Africa will perform vital studies of the fundamental governing electrodynamics of equatorial ionospheric motion. As shown in Figure 3 (blue dots), the AGREES network will contain five GPS receivers which will be deployed at mid- and lowlatitudes in the African continent. The AGREES network will be deployed based on two main priorities that are required for this study. These include: (1) to routinely monitor the strength and evolution of EA region by filling the largest land-based gap of GPS receiver coverage in Africa, (2) to understand the electrodynamics that governs the equatorial ionospheric motion by combining data from GPS receivers network with the already available magnetometer (MAGDAS and AMBER) data.

57

4 IHY/UNBSS Observatory Development Program

60

Geog. Latitude (°N)

40

20

0

–20

–40 –30

–20

–10

0

10

20

30

40

50

60

Geog. Longitude (°E) Fig. 3. European and African ground-based GPS receivers’ network along with proposed AGREES network (blue dots). The circles in each station depict the elevation cut off (15 above the horizontal). The 2-h coverage of eight LEO satellites ground tracks in the region is depicted by different colored triangles.

The ground-based GPS receivers, including AGREES, in the African region will be augmented by data from GPS receivers on board Low-Earth-Orbit (LEO) satellites that are equipped with dual-band GPS receivers. The 2 h coverage of eight LEO satellites (COSMIC, CHAMP, and Jason) in the region is shown in Figure 3. Therefore, the simultaneous application of tomographic reconstruction technique on both ground- and space-based GPS TEC data will allow us to monitor the structure and dynamics of inner-magnetospheric density. This will provide a great opportunity to the scientific community to clearly quantify the dynamics of magnetosphere–ionosphere (M–I) coupling phenomenon. The geographic locations of AGREES stations will be 12.73 S, 15.78 E; 12.11 N, 15.05 E; 17.92 N, 19.12 E; 26.00 N, 14.15 E; and 32.90 N, 13.18 E. Three African countries (Angola, Chad, and Libyan Arab Jamahiriya) will participate in the AGREES project by hosting the GPS receivers. Therefore, 58

4 IHY/UNBSS Observatory Development Program

AGREES project will have direct impact on space science research and education both in African and in the United States by fostering international scientific cooperation. In addition to providing world-class science data to the scientific community, AGREES infrastructure will also provide a self-sustained training and research opportunities in the African universities where space science research activities are rare. In the United States AGREES project will create opportunities for graduate and undergraduate students to do research that will provide them high quality research experiences. The experience will include expertise in data analysis, remote sensing, computer modeling, data assimilation, and grid-based computing and data retrieval.

4.3.1.1.2. AWESOME (Atmospheric Weather Educational System for Observation and Modeling of Effects)

PIs: Umran Inan, Morris Cohen, Deborah Scherrer and Sheila Bijoor, Stanford University The AWESOME instrument is an ionospheric monitor that can be operated by students around the world. The monitors detect solar flares and other ionospheric disturbances. The key elements of the AWESOME are the computer, the Stanford Monitor, and the antenna. The science of AWESOME is central to IHY. The ionosphere is the region of the upper atmosphere where ionization occurs due to solar and cosmic radiation. In the D-region of the ionosphere (50–90 km altitude), the ionization levels are dominated by X-ray flux from the Sun in the daytime, and ambient cosmic-ray flux at night. The D-region is sufficiently ionized as to strongly reflect radio waves in the ELF/VLF range (300–50 kHz), and since the Earth is also highly conducting at these frequencies, these signals can propagate efficiently around the planet in the so-called “Earth-ionosphere waveguide”. Natural ELF/ VLF signals are dominated by the impulsive radiation from lightning strikes, known as radio atmospherics, and can be picked up around the Earth from the source. Since the propagation of these waves in the Earth-ionosphere waveguide is strongly dependent on the ionospheric conditions (being reflected off of the ionosphere), the propagation properties of these waves intrinsically respond to changes in the ionosphere, and are therefore a good diagnostic of ionospheric disturbances. In particular, the nighttime ionosphere is highly variable and poorly understood, but being at a height too high for balloons, too low for satellites, and too lightly ionized for radar measurements, radio measurements such as ELF/VLF constitute one of the few effective means of remote sensing. The ionosphere is known to react to a broad array of geophysical phenomenon, including solar flares, 59

4 IHY/UNBSS Observatory Development Program

lightning, sprites, lightning-induced electron precipitation, cosmic gamma-ray bursts, earthquakes, and more. Studying the ionosphere therefore enables analysis of a broad array of geophysical phenomenon, especially when combined with data from other instruments. AWESOME sensitively detects these ELF/VLF radio waves enabling detailed quantitative analysis of ionospheric conditions. The figure here shows sample ELF/VLF data taken with the AWESOME network. The key elements of the AWESOME are the computer, the Stanford Monitor, and the antenna. An internet link is important; otherwise a good quality DVD burner can be used.

North/South Receiver GPS Receiver

DAQ

Line Receiver Fig. 4. The AWESOME data acquisition system, which works in conjunction with a TrueTime GPS receiver, the line receiver and, the North/South and East/West receivers.

dB-pT 0

40

20.2

-10

20.0

-20

30 19.8 20

-30

19.6

10

-40

19.4 -50

0 20

Picoteslas

NWC (Australia) 20.4

2

Lightning-generated radio atmospheric

10 0 -10

7.90

7.95

8.00

diurnal variations at Stanford

10 -10 -30

200 0 -200

-20 6.266

19.2 7.85

8

6

4

∠A(deg) = |A| (dB-pT)

Frequency (kHz) ΔF = 100 Hz

Stanford ELF/VLF, sec after 10:00 UT, 01-Jun-2008 50

6.268

6.270

6.272

6.274

6.276

Zoomed-in time series plot, sec after 10:00 UT

0

12

24

36

48

60

72

Hours after 2008-Jun-01, 10:00 UT

Fig. 5. Data from the AWESOME instruments allow studies of ionospheric phenomena that would be impossible without ground-based arrays.

60

4 IHY/UNBSS Observatory Development Program

The setup is illustrated in Figure 4. The line receiver gets VLF signals from two antennas. There is usually one antenna in the North/South orientation and another in the East/West orientation. These signals are sent to a 200 kHz ADC card attached to the PCI slot of the computer. The ADC will capture data from each of the two antennas at 100 kHz each. The timing signal from the GPS is also fed into the ADC card, allowing for very precise acquisition of data. Now in development is a USB interface to replace the ADC card, which will enhance the ease of use, and substantially reduce the cost. In Figure 5, the top left plot shows the full 0–50 kHz spectrum, with the color indicating the strength of the magnetic field. The bottom left plot shows an example of a naturally-generated radio atmospheric, originating from a lightning strike which could be anywhere on Earth. The top right plot shows a zoom-in of a VLF transmitter signal from Australia, received at Stanford, California. The digital communication modulation signal is visible in the frequency variations. These steady transmitter signals are excellent diagnostic tools for the ionosphere, since changes in the ionosphere are reflected in the amplitude or phase of this signal. The bottom right plot shows an example of how the transmitter signal, monitored over 3 days, clearly indicates a diurnal pattern dictated by the day/night ionospheric variation along the transmitterto-receiver path. Because of its broad application for studying a wide variety of geophysical phenomenon via the method of VLF remote sensing, relative ease of data analysis,

IHY Distribution 2007–2009

Larger dots indicate multiple sites

Fig. 6. Map of AWESOME and SID monitors. Ten additional monitors are expected to be complete by the middle of 2009.

61

4 IHY/UNBSS Observatory Development Program

and its comparatively low-cost within the realm of scientific instruments, the AWESOME is well suited for extension to a global network under the IHY program. Under the umbrella of the IHY program, 29 AWESOMEs have been distributed worldwide, with another 10 planned by the middle of 2009. Figure 6 shows these sites (blue dots represent AWESOME placements). We build on this global AWESOME network to establish radio science expertise at underdeveloped sites by (1) creating a collection of online tools to enable advanced data analysis, and (2) developing initiatives to promote mentorship and collaboration amongst sites. The first of these tools is the AWESOME Online Data Viewer, a web-accessible interface that allows users to map ELF/VLF wave propagation along global paths, graph data, and easily share and download images. Another tool, known as the AWESOME Collaborative Forum, is an online forum for international researchers to collect scientific information, share discoveries, and foster new collaborations. We are currently developing a web-accessible AWESOME ELF/VLF Science Tutorial Series to educate new scientists about the breadth of VLF research topics. In Fall 2008, Stanford conducted a series of regional Workshops dedicated to promoting science cooperation amongst sites. The Workshops consisted of invited research lectures, hands-on data tutorials, collaborative research activities, and interactive networking sessions to fully enable new ELF/VLF researchers to utilize their VLF data for advanced and meaningful scientific research. The goal of these workshops is to establish collaborative projects resulting in published papers in refereed scientific journals. With the first papers already in development, and the current and next round of site deployments now developing their own expertise and project ideas, we expect the AWESOMEs impact on global science to grow in the coming years. We intend for these workshops to culminate in a series of annual or twice-per-year fully international workshops in which these IHY/AWESOME collaborative links can be further nurtured, and new/exciting results presented to the community. The IHY recognizes that, in order to develop space science research infrastructure in Developing Nations, space science education must also be improved to support the long-term operation and use of scientific instrumentation. The AWESOME project includes an educational component designed to address this need. Inexpensive student versions of the monitors, less sensitive, were developed and distributed worldwide through the Stanford Solar Center. These student instruments, called Sudden Ionospheric Disturbance monitors (SIDs), provide similar capability to the AWESOMEs though focus primarily on the influence of solar activity upon the ionosphere. The distribution kit includes extensive curricula and backgound information which were designed to inspire and engage the next generation of space scientists. Over 300 SID instruments have 62

4 IHY/UNBSS Observatory Development Program

been distributed for the IHY (red dots on map). The SIDs are described in more detail in the education section (Sect. 5) of this report.

4.3.1.1.3. GPS in Africa

PIs: Christine Amory-Mazaudier, Monique Petitdidier, and Paul Vila (CNES, France), Tim Fuller-Rowell (University of Colorado and NOAA Space Environment Center), Sunanda Basu (Boston University). Much attention in space weather has been devoted recently to the large changes in total electron content (TEC) over the American sector during geomagnetic storms. The attention has been fueled by the ability to map the electron content using networks of ground-based, dual-frequency GPS receivers. Figure 7 shows a large gradient in TEC stretching across the Eastern United States during an ionospheric storm, driven by electrodynamics. Steep gradients in TEC can disrupt operational systems such as the Wide Area Augmentation System (WAAS), which is utilized by the Federal Aviation Administration (FAA) for aircraft positioning. This gradient severely disrupted the FAA use of WAAS over its service volume for periods totaling 26 h navigation errors sometimes exceeded 50 m more than 10 times typical uncertainties of 2–3 m. The Geomagnetic Field: There has been speculation that the large change in plasma density and electrodynamics in the American sector is related to the unusual configuration of the geomagnetic field, including the South Atlantic Anomaly (SAA) and large values of declination. The speculation has spurred the need to target other geographic regions with significantly different geomagnetic field configurations. In contrast, over Africa the magnetic equator is parallel to the geographic equator and more uniform in magnitude. This region, however, does

November 20, 2003 20:30 UT

CTIP_APEX:TEC (m-2): Equinox, F10 180., OUT

log TEC (TECu) 90

2

50

1.2E+18

60

1.8

45

1.6

40 35

1.4 1.2

30 25

1

20 15 10 –120 –110 –100

–90

–80

West longitude

–70

–60

9.0E+17

Latitude

60 55

30

6.0E+17

0

–30

3.0E+17

0.8

–60

0.6

–90

0

0.0E+00 6

12

18

24

Local time

Fig. 7. Left: Example of a plume of storm enhanced density derived from GPS “imaging” (J. Foster, private communication). Right: Illustration of the distortion of the geomagnetic field between the American and African sectors.

63

4 IHY/UNBSS Observatory Development Program

not have a dense network of ground-based GPS receivers available to perform a complementary study, nor does it have sufficient magnetometer chains to monitor the dayside plasma drift. Objective: The observations over Africa will be used to determine the source of the plasma bulge at midlatitudes that provide the seed for the plume seen in Figure 7. The plasma bulge can either be created in-situ as a natural consequence of the expansion of the high latitude magnetospheric convection pattern to low latitudes, or is formed by transporting plasma from low latitudes. The latter mechanism relies on strong meridional and zonal plasma transport from the equatorial ionization anomaly (EIA) in the presence of the distortion of the geomagnetic field. Observation over Africa, with the much more uniform magnetic field, provide an excellent test for the two theories. The space science community is therefore exploring ways to increase the observational infrastructure at mid and low latitudes over the African continent. The GPS in Africa project is therefore collaborating with other activities in the region, such as the Multidisciplinary Analysis of the Monsoon in Africa (AMMA), the CARISMA Project (Ian Mann) and the SCINDA project (Keith Groves), in order to provide the necessary spatial coverage. In addition, we would like to encourage scientists in the African Universities to become interested in the science objectives and be willing to host a dual-frequency GPS system at their Universities. Unraveling the physical processes controlling the redistribution of plasma requires coordinating the ionospheric observations over the African continent and assembling the information in a common database. The observations from the common database can be used to address a range of science questions under the IHY-Africa initiative.

4.3.1.1.4. ITNE (Ionospheric Tomography Network of Egypt)

PIs: Ayman Mahrous (Helwan University, Egypt) and Trevor Garner (University of Texas at Austin, USA) ITNE is a network of Coherent Ionospheric Doppler Receivers (CIDR). A CIDR system installation consists of the CIDR receiver, a control computer (which is provided with the system, typically a laptop) and two antennas (one for CIDR, one GPS). The antenna installation requires a good all-sky view with minimal or no obstructions. 100-m cables are provided as well. An internet connection allows each individual CIDR system to be accessed by the science team remotely. The internet connection will also be used to download satellite track information (so that the system may plan which satellite passes it can observe and record) and the collected data is uploaded to archives for use by the science team. If there is a broadband connection, individual satellite passes can be remotely monitored via a web interface. 64

4 IHY/UNBSS Observatory Development Program

As part of the IHY effort to increase the ionospheric instrumentation in Africa, Helwan University in Helwan, Egypt and the Applied Research Laboratories: The University of Texas at Austin (ARL:UT) have teamed up with other Egyptian universities to develop the Ionospheric Tomography Network of Egypt (ITNE). ITNE is a chain of three UHF/VHF Doppler receivers distributed at different universities throughout Egypt (see Table 1). It is a roughly north–south chain (like  much of Egypt, it is aligned with the Nile river). ITNE stretches from 24 to  15 magnetic latitude, and sits under the northern peak of the equatorial anomaly. The first receiver system is operational with the two additional systems (already in Egypt) coming on line in the near future. INTE provides a new and valuable data set to study the equatorial anomaly in the African sector. Coherent Ionospheric Doppler Receiver systems will be the primary observing system for this study. CIDRs, developed at ARL:UT, are radio receivers designed to measure the line-of-sight, relative TEC using the 150 and 400 MHz radio beacons on board LEO satellites. Figure 8 shows the standard CIDR system. The fundamental CIDR measurement is the Doppler shift in each channel. By downconverting each signal to a common frequency and subtracting the Doppler shifts, the rate of TEC (ROT) change, dTEC/dt, can be derived and integrated to produce a relative TEC. These are line-of-sight measurements with measurements from other receivers can be combined through different tomographic and data assimilative techniques to reconstruct two- or three-dimensional electron density distributions.

Fig. 8. A photo of a CIDR system with its individual components. From left to right, the components are the UHF/VHF antenna, the receiver, and the laptop.

65

4 IHY/UNBSS Observatory Development Program

Since the low-Earth orbiting (LEO) spacecraft (800–1000 km apogee) cross the receiver’s field-of-view in only a few minutes (typically 20 min), these measurements fundamentally show spatial variations in the electron content. In contrast, GPS satellites take 8 h to cross a ground receiver’s field-of-view, making GPS TEC measurements a better measurement of temporal changes in the ionosphere than of spatial changes. In addition, LEO spacecraft fly completely within the ionosphere so the observed TEC consists solely ionospheric plasma (GPS TEC measurements contain plasmaspheric plasma as well). The data rate in CIDR equipment is higher than in typical GPS receivers. CIDRs typically take measurements at 1 Hz and can take data as high at 1 kHz, a higher data rate than a typical GPS receiver (every 30 s). With fourteen available beacon satellites, CIDR systems operate nearly continuously with typical data gaps of less than 60 min. As such, CIDR systems will provide a high quality data set for observing the equatorial ionosphere. A CIDR is capable of tracking up to three different beacon satellites with different frequency offsets at one time, including the Navy Ionospheric Monitoring System (NIMS) operational and maintenance offsets, and any LEO satellite operating on the “geodetic” channel. Currently, there are four NIMS satellites and ten geodetics spacecraft that CIDR can track. In addition to tracking a large number of satellites and the ability to track multiple satellites simultaneously, CIDR has a number of other capabilities including: * * *

Relative Slant TEC (TECu/s)

*

User selectable sampling rates as high as 1 kHz; Instrument error of